It is still unknown whether the mass terms for neutrinos are of Majorana type
or of Dirac type. An interesting possibility, known as pseudo-Dirac scheme
combines these two with a dominant Dirac mass term and a subdominant Majorana
one. As a result, the mass eigenstates come in pairs with a maximal mixing and
a small splitting determined by the Majorana mass. This will affect the
neutrino oscillation pattern for long baselines. We revisit this scenario
employing recent solar neutrino data, including the seasonal variation of the
$^7$Be flux recently reported by BOREXINO. We constrain the splitting using
these data and find that both the time integrated solar neutrino data and the
seasonal variation independently point towards a new pseudo-Dirac solution with
nonzero splitting for $\nu_2$ of $\Delta m_2^2\simeq 1.5\times 10^{-11}$
eV$^2$. We propose alternative methods to test this new solution. In
particular, we point out the importance of measuring the solar neutrino flux at
the intermediate energies $1.5~{\rm MeV}
Entanglement in three-flavor collective neutrino oscillations
2211.07678 [abs] [pdf]
[abstract]
by Pooja Siwach, Anna M. Suliga, and A. Baha Balantekin.
Extreme conditions present in the interiors of the core-collapse supernovae
make neutrino-neutrino interactions not only feasible but dominant in specific
regions, leading to the non-linear evolution of the neutrino flavor. Results
obtained when such collective neutrino oscillations are treated in the
mean-field approximation deviate from the results using the many-body picture
because of the ignored quantum correlations. We present the first three flavor
many-body calculations of the collective neutrino oscillations. The
entanglement is quantified in terms of the entanglement entropy and the
components of the polarization vector. We propose a qualitative measure of
entanglement in terms of flavor-lepton number conserved quantities. We find
that in the cases considered in the present work, the entanglement can be
underestimated in two flavor approximation. The dependence of the entanglement
on mass ordering is also investigated. We also explore the mixing of mass
eigenstates in different mass orderings.
Can ultralight dark matter explain the age-velocity dispersion relation
of the Milky Way disc: A revised and improved treatment
2211.07452 [abs] [pdf]
[abstract]
by Barry T. Chiang, Jeremiah P. Ostriker, and Hsi-Yu Schive.
Ultralight axion-like particles $m_a \sim 10^{-22}$ eV, or Fuzzy Dark Matter
(FDM), behave comparably to cold dark matter (CDM) on cosmological scales and
exhibit a kpc-size de Broglie wavelength capable of alleviating established
(sub-)galactic-scale problems of CDM. Substructures inside an FDM halo incur
gravitational potential perturbations, resulting in stellar heating sufficient
to account for the Galactic disc thickening over a Hubble time, as first
demonstrated by Church et al. We present a more sophisticated treatment that
incorporates the full baryon and dark matter distributions of the Milky Way and
adopts stellar disc kinematics inferred from recent Gaia, APOGEE, and LAMOST
surveys. Ubiquitous density granulation and subhalo passages respectively drive
inner disc thickening and flaring of the outer disc, resulting in an
observationally consistent `U-shaped' disc vertical velocity dispersion profile
with the global minimum located near the solar radius. The observed
age-velocity dispersion relation in the solar vicinity can be explained by the
FDM-substructure-induced heating and places an exclusion bound $m_a \gtrsim
0.4\times10^{-22}$ eV. We assess non-trivial uncertainties in the empirical
core-halo relation, FDM subhalo mass function and tidal stripping, and stellar
heating estimate. The mass range $m_a\simeq 0.5-0.7\times10^{-22}$ eV favoured
by the observed thick disc kinematics is in tension with several exclusion
bounds inferred from dwarf density profiles, stellar streams, and Milky Way
satellite populations, which could be significantly relaxed due to the
aforesaid uncertainties. Additionally, strongly anisotropic heating could help
explain the formation of ultra-thin disc galaxies.
Wilks's Theorem, Global Fits, and Neutrino Oscillations
2211.06347 [abs] [pdf]
[abstract]
by J. M. Hardin.
Tests of models for new physics appearing in neutrino experiments often
involve global fits to a quantum mechanical effect called neutrino
oscillations. This paper introduces students to methods commonly used in these
global fits starting from an understanding of more conventional fitting methods
using log-likelihood and $\chi^2$ minimization. Specifically, we discuss how
the $\Delta\chi^2$, which compares the $\chi^2$ of the fit with the new physics
to the $\chi^2$ of the Standard Model prediction, is often interpreted using
Wilks's theorem. This paper uses toy models to explore the properties of
$\Delta\chi^2$ as a test statistic for oscillating functions. The statistics of
such models are shown to deviate from Wilks's theorem. Tests for new physics
also often examine data subsets for ``tension'' called the ``parameter goodness
of fit''. In this paper, we explain this approach and use toy models to examine
the validity of the probabilities from this test also. Although we have chosen
a specific scenario -- neutrino oscillations -- to illustrate important points,
students should keep in mind that these points are widely applicable when
fitting multiple data sets to complex functions.
Studying neutrino oscillations at DUNE through dynamical Lorentz
symmetry breaking in four-Majorana fermion model
2211.06192 [abs] [pdf]
[abstract]
by Susie Kim.
We study the impact of the dynamical Lorentz symmetry breaking induced by the
auxiliary gauge fields of neutrino on the oscillations probability at DUNE. The
DLSB introduces an alternative energy-momentum relation of the neutrinos and
thus results in a new oscillation probability. We extend the previously
proposed four-Majorana fermion model that gives rise to DLSB after the type II
seesaw mechanism by considering the electron neutrino forward scattering when
passing through a medium. Moreover, we incorporate the three-flavor neutrino
states, which introduce the CP-violation term inside the oscillation
probability. The impact of DLSB parameters around the order of
$10^{-2}-10^{-3}$, which are at a strong coupling regime, on the oscillation
probability is found to be measurable at DUNE within the 20 years through
$\nu_e$ and $\overline{\nu}_e$ disappearance signals. We also compare the
predicted spectra of the DLSB oscillations and the oscillation with the
CP-violating term equal to $\pi/2$ to conclude that the presence of DLSB would
increase the systematic uncertainty for the measurement of CP-violation at
DUNE.
Updated constraints on sterile neutrino mixing in the OPERA experiment
using a new $ν_e$ identification method
2211.04636 [abs] [pdf]
[abstract]
by N. Agafonova, [and 125 more]A. Alexandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, A. Bertolin, C. Bozza, R. Brugnera, S. Buontempo, M. Chernyavskiy, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievsky, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, V. Gentile, J. Goldberg, S. Gorbunov, Y. Gornushkin, G. Grella, A. M. Guler, C. Gustavino, C. Hagner, T. Hara, T. Hayakawa, A. Hollnagel, K. Ishiguro, A. Iuliano, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, F. Laudisio, A. Lauria, A. Longhin, P. Loverre, A. Malgin, G. Mandrioli, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, S. Mikado, M. Miyanishi, F. Mizutani, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, K. Niwa, S. Ogawa, N. Okateva, K. Ozaki, A. Paoloni, L. Paparella, B. D. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, T. Roganova, H. Rokujo, G. Rosa, O. Ryazhskaya, O. Sato, A. Schembri, I. Shakiryanova, T. Shchedrina, E. Shibayama, H. Shibuya, T. Shiraishi, S. Simone, C. Sirignano, G. Sirri, A. Sotnikov, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, S. Vasina, P. Vilain, E. Voevodina, L. Votano, J. L. Vuilleumier, G. Wilquet, and C. S. Yoon [hide authors].
This paper describes a new $\nu_e$ identification method specifically
designed to improve the low-energy ($< 30\,\mathrm{GeV}$) $\nu_e$
identification efficiency attained by enlarging the emulsion film scanning
volume with the next generation emulsion readout system. A relative increase of
25-70% in the $\nu_e$ low-energy region is expected, leading to improvements in
the OPERA sensitivity to neutrino oscillations in the framework of the 3 + 1
model. The method is applied to a subset of data where the detection efficiency
increase is expected to be more relevant, and one additional $\nu_e$ candidate
is found. The analysis combined with the $\nu_\tau$ appearance results improves
the upper limit on $\sin^2 2\theta_{\mu e}$ to 0.016 at 90% C.L. in the
MiniBooNE allowed region $\Delta m^2_{41} \sim 0.3\,\mathrm{eV}^2$.
The ngEHT's Role in Measuring Supermassive Black Hole Spins
2211.03910 [abs] [pdf]
[abstract]
by Angelo Ricarte, [and 4 more]Paul Tiede, Razieh Emami, Aditya Tamar, and Priyamvada Natarajan [hide authors].
While supermassive black hole masses have been cataloged across cosmic time,
only a few dozen of them have robust spin measurements. By extending and
improving the existing Event Horizon Telescope (EHT) array, the next-generation
Event Horizon Telescope (ngEHT) will enable multifrequency, polarimetric movies
on event horizon scales, which will place new constraints on the space-time and
accretion flow. By combining this information, it is anticipated that the ngEHT
may be able to measure tens of supermassive black hole masses and spins. In
this white paper, we discuss existing spin measurements and many proposed
techniques with which the ngEHT could potentially measure spins of target
supermassive black holes. Spins measured by the ngEHT would represent a
completely new sample of sources that, unlike pre-existing samples, would not
be biased towards objects with high accretion rates. Such a sample would
provide new insights into the accretion, feedback, and cosmic assembly of
supermassive black holes.
$γ$-ray and ultra-high energy neutrino background suppression due
to solar radiation
2211.03807 [abs] [pdf]
[abstract]
by Shyam Balaji.
The Sun emits copious amounts of photons and neutrinos in an approximately
spatially isotropic distribution. Diffuse $\gamma$-rays and ultra-high energy
(UHE) neutrinos from extragalactic sources may subsequently interact and
annihilate with the emitted solar photons and neutrinos respectively. This will
in turn induce an anisotropy in the cosmic ray background due to attenuation of
the $\gamma$-ray and UHE neutrino flux by the solar radiation. Measuring this
reduction, therefore, presents a simple and powerful astrophysical probe of
electroweak interactions. In this letter we compute such anisotropies, which at
the Earth (Sun) can be $\simeq 2\times 10^{-3}\,(0.5)\%$ and $\simeq 1\times
10^{-16}\,(2\times 10^{-14})\%$ for TeV scale $\gamma$-rays and PeV scale UHE
neutrinos respectively. We briefly discuss exciting observational prospects for
experiments such as the Fermi Gamma-Ray Space Telescope Large Area Telescope
(Fermi LAT), High Energy Stereoscopic System (H.E.S.S), High-Altitude Water
Cherenkov (HAWC) detector and IceCube. The potential for measuring $\gamma$-ray
attenuation at orbital locations of other active satellites such as the Parker
Solar Probe and James Webb Space Telescope is also explored.
Sterile Neutrinos: Propagation in Matter and Sensitivity to Sterile Mass
Ordering
2211.03473 [abs] [pdf]
[abstract]
by Dibya S. Chattopadhyay, [and 5 more]Moon Moon Devi, Amol Dighe, Debajyoti Dutta, Dipyaman Pramanik, and Sushant K. Raut [hide authors].
We analytically calculate the neutrino conversion probability $P_{\mu e}$ in
the presence of sterile neutrinos, with exact dependence on $\Delta m^2_{41}$
and with matter effects explicitly included. Using perturbative expansion in
small parameters, the terms involving the small mixing angles $\theta_{24}$ and
$\theta_{34}$ can be separated out, with $\theta_{34}$ dependence only arising
due to matter effects. We express $P_{\mu e}$ in terms of the quantities of the
form $\sin(x)/x$, which helps in elucidating its dependence on matter effects
and a wide range of $\Delta m^2_{41}$ values. Our analytic expressions allow us
to predict the effects of the sign of $\Delta m^2_{41}$ at a long baseline
experiment like DUNE. We numerically calculate the sensitivity of DUNE to the
sterile mass ordering and find that this sensitivity can be significant in the
range $|\Delta m^2_{41}| \sim (10^{-4} - 10^{-2})$ eV$^2$, for either mass
ordering of active neutrinos. The dependence of this sensitivity on the value
of $\Delta m^2_{41}$ for all mass ordering combinations can be explained by
investigating the resonance-like terms appearing due to the interplay between
the sterile sector and matter effects.
Measuring Oscillations with A Million Atmospheric Neutrinos
2211.02666 [abs] [pdf]
[abstract]
by C. A. Argüelles, [and 3 more]P. Fernández, I. Martínez-Soler, and M. Jin [hide authors].
We analyze the expected sensitivity of current and near-future
water(ice)-Cherenkov atmospheric neutrino experiments in the context of
standard three-flavor neutrinos oscillations. In this first in-depth combined
atmospheric neutrino analysis, we analyze the current shared systematic
uncertainties arising from the shared flux and neutrino-water interactions. We
then implement the systematic uncertainties of each experiment in detail and
develop the atmospheric neutrino simulations for Super-Kamiokande (SK), with
and without neutron-tagging capabilities (including SuperK-Gd),
IceCube-Upgrade, and ORCA detectors. We carefully review the synergies and
features of these experiments to examine the potential of a joint analysis of
these atmospheric neutrino data in resolving the $\theta_{23}$ octant at 99\%
C.L. and determining the neutrino mass ordering above 5$\sigma$ by 2030.
Additionally, we assess the capability to constraint $\theta_{13}$ and the
CP-violating phase ($\delta_{CP}$) in the leptonic sector independently from
reactor and accelerator neutrino data, providing vital information for
next-generation neutrino oscillation experiments such as DUNE and
Hyper-Kamiokande.
New Clues About Light Sterile Neutrinos: Preference for Models with
Damping Effects in Global Fits
2211.02610 [abs] [pdf]
[abstract]
by J. M. Hardin, [and 7 more]I. Martinez-Soler, A. Diaz, M. Jin, N. W. Kamp, C. A. Argüelles, J. M. Conrad, and M. H. Shaevitz [hide authors].
This article reports global fits of short-baseline neutrino data to
oscillation models involving light sterile neutrinos. In the commonly-used 3+1
plane wave model, there is a well-known 4.9$\sigma$ tension between data sets
sensitive to appearance versus disappearance of neutrinos. We find that models
that damp the oscillation prediction for the reactor data sets, especially at
low energy, substantially improve the fits and reduce the tension. We consider
two such scenarios. The first scenario introduces the quantum mechanical
wavepacket effect that accounts for the source size in reactor experiments into
the 3+1 model. We find that inclusion of the wavepacket effect greatly improves
the overall fit compared to a 3$\nu$ model by $\Delta \chi^2/$DOF$=61.1/4$
($7.1\sigma$ improvement) with best-fit $\Delta m^2=1.4$ eV$^2$ and wavepacket
length of 67fm. The internal tension is reduced to 3.4$\sigma$. If reactor-data
only is fit, then the wavepacket preferred length is 91 fm ($>20$ fm at 99\%
CL). The second model introduces oscillations involving sterile flavor and
allows the decay of the heaviest, mostly sterile mass state, $\nu_4$. This
model introduces a damping term similar to the wavepacket effect, but across
all experiments. Compared to a three-neutrino fit, this has a $\Delta
\chi^2/$DOF$=60.6/4$ ($7\sigma$ improvement) with preferred $\Delta m^2=1.4$
eV$^2$ and decay $\Gamma = 0.35$ eV$^2$. The internal tension is reduced to
3.7$\sigma$.
For many years, the reactor event rates have been observed to have structure
that deviates from prediction. Community discussion has focused on an excess
compared to prediction observed at 5 MeV; however, other deviations are
apparent. This structure has $L$ dependence that is well-fit by the damped
models. Before assuming this points to new physics, we urge closer examination
of systematic effects that could lead to this $L$ dependence.
Neutrino Origin of LHAASO's 18 TeV GRB221009A Photon
2211.02028 [abs] [pdf]
[abstract]
by Vedran Brdar and Ying-Ying Li.
LHAASO collaboration detected photons with energy above 10 TeV from the most
recent gamma-ray burst (GRB), GRB221009A. Given the redshift of this event,
$z\sim 0.15$, photons of such energy are expected to interact with the diffuse
extragalactic background light (EBL) well before reaching Earth. In this paper
we provide a novel neutrino-related explanation of the most energetic 18 TeV
event reported by LHAASO. We find that the minimal viable scenario involves
both mixing and transition magnetic moment portal between light and sterile
neutrinos. The production of sterile neutrinos occurs efficiently via mixing
while the transition magnetic moment portal governs the decay rate in the
parameter space where tree-level decays via mixing to non-photon final states
are suppressed. Our explanation of this event, while being consistent with the
terrestrial constraints, points to the non-standard cosmology.
On ALP scenarios and GRB 221009A
2211.02010 [abs] [pdf]
[abstract]
by Pierluca Carenza and M. C. David Marsh.
The extraordinarily bright gamma-ray burst GRB 221009A was observed by a
large number of observatories, from radio frequencies to gamma-rays. Of
particular interest are the reported observations of photon-like air showers of
very high energy: an 18 TeV event in LHAASO and a 251 TeV event at Carpet-2.
Gamma rays at these energies are expected to be absorbed by pair-production
events on background photons when travelling intergalactic distances. Several
works have sought to explain the observations of these events, assuming they
originate from GRB 221009A, by invoking axion-like particles (ALPs). We
reconsider this scenario and account for astrophysical uncertainties due to
poorly known magnetic fields and background photon densities. We find that,
robustly, the ALP scenario cannot simultaneously account for an 18 TeV and a
251 TeV photon from GRB 221009A.
Study of light sterile neutrino at the long-baseline experiment options
at KM3NeT
2211.01816 [abs] [pdf]
[abstract]
by Dinesh Kumar Singha, [and 3 more]Monojit Ghosh, Rudra Majhi, and Rukmani Mohanta [hide authors].
In this paper, we study the capability of different long-baseline experiment
options at the KM3NeT facility i.e., P2O, Upgraded P2O and P2SO to probe the
light sterile neutrino and compare their sensitivities with DUNE. The P2O
option will have neutrinos from a 90 KW beam at Protvino to be detected at the
ORCA detector, the Upgraded P2O will have neutrinos from the upgraded 450 KW
beam to be detected at the ORCA detector and the option P2SO will have
neutrinos from a 450 KW beam to be detected at the upgraded Super-ORCA
detector. All these options will have a baseline around 2595 km. Our results
show that the experiments at the KM3NeT (DUNE) would be more sensitive if the
value of $\Delta m^2_{41}$ is around 10 (1) eV$^2$. Our results also show that
the role of near detector is very important for the study of sterile neutrinos
and addition of near detector improves the sensitivity as compared to only far
detector for 3+1 scenario. Among the three options at KM3NeT, the sensitivity
of P2O and upgraded P2O is limited and sensitivity of P2SO is either comparable
or better than DUNE.
A seesaw model for large neutrino masses in concordance with cosmology
2211.01729 [abs] [pdf]
[abstract]
by Miguel Escudero, Thomas Schwetz, and Jorge Terol-Calvo.
Cosmological constraints on the sum of the neutrino masses can be relaxed if
the number density of active neutrinos is reduced compared to the standard
scenario, while at the same time keeping the effective number of neutrino
species $N_{\rm eff}\approx 3$ by introducing a new component of dark
radiation. We discuss a UV complete model to realise this idea, which
simultaneously provides neutrino masses via the seesaw mechanism. It is based
on a $U(1)$ symmetry in the dark sector, which can be either gauged or global.
In addition to heavy seesaw neutrinos, we need to introduce $\mathcal{O}(10)$
generations of massless sterile neutrinos providing the dark radiation. Then we
can accommodate active neutrino masses with $\sum m_\nu \sim 1$ eV, in the
sensitivity range of the KATRIN experiment. We discuss the phenomenology of the
model and identify the allowed parameter space. We argue that the gauged
version of the model is preferred, and in this case the typical energy scale of
the model is in the 10 MeV to few GeV range.
GRB 221009A Gamma Rays from Radiative Decay of Heavy Neutrinos?
2211.00634 [abs] [pdf]
[abstract]
by Alexei Y. Smirnov and Andreas Trautner.
We consider a mechanism which allows to decrease attenuation of high energy
gamma ray flux from gamma ray burst GRB 221009A. The mechanism is based on the
existence of a heavy $m_N\sim0.1\,\mathrm{MeV}$ mostly sterile neutrino $N$
which mixes with active neutrinos. $N$'s are produced in GRB in $\pi$ and $K$
decays via mixing with $\nu_\mu$. They undergo the radiative decay
$N\rightarrow \nu \gamma$ on the way to the Earth. The usual exponential
attenuation of gamma rays is lifted to an attenuation inverse in the optical
depth. Various restrictions on this scenario are discussed. We find that the
high energy $\gamma$ events at $18\,\mathrm{TeV}$ and potentially
$251\,\mathrm{TeV}$ can be explained if (i) the GRB active neutrino fluence is
close to the observed limit, (ii) the branching ratio of $N\rightarrow \nu
\gamma$ is at least of the order 10%.
Probe the Mixing Parameter $|V_{τN}|^2$ for Heavy Neutrinos
2211.00309 [abs] [pdf]
[abstract]
by Lingxiao Bai, Ying-nan Mao, and Kechen Wang.
Because of the difficulty in detecting final state taus, the mixing parameter
$|V_{\tau N}|^2$ for heavy neutrino $N$ is not well studied at current
experiments, compared with other mixing parameters $|V_{e N}|^2$ and $|V_{\mu
N}|^2$. In this paper, we focus on a challenging scenario where $N$ mixes with
active neutrino of tau flavour only, i.e. $ |V_{\tau N}|^2 \neq 0 $ and $|V_{e
N}|^2 = |V_{\mu N}|^2 = 0$. We derive current constraints on $|V_{\tau N}|^2$
from the rare $Z$-boson decay and electroweak precision data (EWPD). To
forecast the future limits, we also investigate the signal $p p \to \tau^{\pm}
\tau^{\pm} j j $ via a Majorana heavy neutrino at future proton-proton
colliders. To suppress the background, both taus are required to decay
leptonically into muons, leading to the final state containing two same sign
muons, at least two jets plus moderate missing energy. The signal and relevant
background processes are simulated at the HL-LHC and SppC/FCC-hh with
center-of-mass energy of 14 TeV and 100 TeV. The preselection and multivariate
analyses based on machine-learning are performed to reduce background. Limits
on $|V_{\tau N}|^2$ are shown for heavy neutrino mass in the range 10-1000 GeV
based on measurements from the rare $Z$-boson decay and EWPD, and searches at
the HL-LHC and SppC/FCC-hh with integrated luminosities of 3 and 20 ab$^{-1}$.
October 2022
Neutrinos from the Brightest Gamma-Ray Burst?
2210.15625 [abs] [pdf]
[abstract]
by Kohta Murase, [and 4 more]Mainak Mukhopadhyay, Ali Kheirandish, Shigeo S. Kimura, and Ke Fang [hide authors].
We discuss implications that can be obtained by searches for neutrinos from
the brightest gamma-ray burst, GRB 221009A. We derive constraints on GRB model
parameters such as the cosmic-ray loading factor and dissipation radius, taking
into account both neutrino spectra and effective areas. The results are strong
enough to constrain proton acceleration near the photosphere, and we find that
the single burst limits are comparable to those from stacking analysis.
Quasithermal neutrinos from subphotospheres and ultrahigh-energy neutrinos from
external shocks are not yet constrained. We show that GeV-TeV neutrinos
originating from neutron collisions are detectable, and urge dedicated analysis
on these neutrinos with DeepCore and IceCube as well as ORCA and KM3NeT.
NaNu: Proposal for a Neutrino Experiment at the SPS Collider located at
the North Area of CERN
2210.15532 [abs] [pdf]
[abstract]
by Friedemann Neuhaus, [and 3 more]Matthias Schott, Chen Wang, and Rainer Wanke [hide authors].
Several experiments have been proposed in the recent years to study the
nature of tau neutrinos, in particular aiming for a first observation of tau
anti-neutrinos, more stringent upper limit on its anomalous magnetic moment as
well as new constrains on the strange-quark content of the nucleon. We propose
here a new low-cost neutrino experiment at the CERN North area, named NaNu
(North Area NeUtrino), compatible with the realization of the future SHADOWS
and HIKE experiments at the same experimental area.
A Significant Sudden Ionospheric Disturbance associated with Gamma-Ray
Burst GRB 221009A
2210.15284 [abs] [pdf]
[abstract]
by Laura A. Hayes and Peter T. Gallagher.
We report the detection of a significant ionospheric disturbance in the
D-region of Earth's ionosphere which was associated with the massive gamma-ray
burst GRB 221009A that occurred on October 9 2022. We identified the
disturbance over northern Europe - a result of the increased ionisation by X-
and gamma-ray emission from the GRB - using very low frequency (VLF) radio
waves as a probe of the D-region. These observations demonstrate that an
extra-galactic GRB can have a significant impact on the terrestrial ionosphere
and illustrates that the Earth's ionosphere can be used as a giant X- and
gamma-ray detector. Indeed, these observations may provide insights into the
impacts of GRBs on the ionospheres of planets in our solar system and beyond.
Neutral-current neutrino cross section and expected supernova signals
for $^{40}$Ar from a three-fold increase in the magnetic dipole strength
2210.14316 [abs] [pdf]
[abstract]
by W. Tornow, [and 7 more]A. P. Tonchev, S. W. Finch, Krishichayan, X. B. Wang, A. C. Hayes, H. G. D. Yeomans, and D. A. Newmark [hide authors].
In view of the great interest in liquid argon neutrino detectors, the
$^{40}$Ar($\gamma,\gamma'$)$^{40}$Ar$^{*}$ reaction was revisited to guide a
calculation of the neutral current neutrino cross section at supernova
energies. Using the nuclear resonance fluorescence technique with a
monoenergetic, 99% linearly polarized photon beam, we report a three-fold
increase in magnetic dipole strength at around 10 MeV in $^{40}$Ar. Based on
shell-model calculations, and using the experimentally identified transitions,
the neutral current neutrino cross sections for low-energy reactions on
$^{40}$Ar are calculated.
The Role of a Heavy Neutrino in the Gamma-Ray Burst GRB-221009A
2210.14178 [abs] [pdf]
[abstract]
by Kingman Cheung.
Recently, several telescopes, including Swift-BAT, GBM, and LHAASO, have
observed the ever highest-energy and long-duration gamma-rays from a gamma-ray
burst named as GRB221009A (located at a red-shift of $z=0.151$) on October 9,
2022. Conventional understanding tells us that very high-energy photons
produced at such a far distance suffer severe attenuation before reaching the
Earth. We propose the existence of a sub-MeV to $O(10)$ MeV heavy neutrino with
a transitional magnetic dipole moment, via which the heavy neutrino is produced
at the GRB. It then travels a long distance to our galaxy and decays into a
neutrino and a photon, which is observed. In such a way, the original
high-energy photon produced at the GRB can survive long-distance attenuation.
Stringent constraint on CPT violation with the synergy of T2K-II,
NO$ν$A extension, and JUNO
2210.13044 [abs] [pdf]
[abstract]
by T. V. Ngoc, [and 3 more]S. Cao, N. T. Hong Van, and P. T. Quyen [hide authors].
Neutrino oscillation experiments have measured precisely the mass-squared
differences of three neutrino mass eigenstates, and three leptonic mixing
angles by utilizing both neutrino and anti-neutrino oscillations. The possible
CPT violation may manifest itself in the difference of neutrino and
anti-neutrino oscillation parameters, making these experiments promising tools
for testing CPT invariance. We investigate empirically the sensitivity of the
CPT test via the difference in mass-squared splittings ($\Delta m^2_{31} -
\Delta \overline{m}^2_{31}$) and in leptonic mixing angles ($\sin^2\theta_{23}
- \sin^2\overline{\theta}_{23}$) with the synergy of T2K-II, NO$\nu$A
extension, and JUNO experiments. If the CPT symmetry is found to be conserved,
the joint analysis of the three experiments will be able to establish limits of
$|\Delta m^2_{31} - \Delta \overline{m}^2_{31}|$ < $5.3\times 10^{-3}
\text{eV}^2$ and $|\sin^2\theta_{23} - \sin^2\overline{\theta}_{23}|$ < $0.10$
at 3$\sigma$ C. L. on the possible CPT violation. We find that with ($\Delta
m^2_{31} - \Delta \overline{m}^2_{31}$), the dependence of the statistical
significance on the relevant parameters to exclude the CPT conservation is
marginal, and that, if the difference in the best-fit values of $\Delta
m^2_{31}$ and $\Delta \overline{m}^2_{31}$ measured by MINOS(+) and NO$\nu$A
persists as the true, the combined analysis will rule out the CPT conservation
at 4$\sigma$ C. L.. With the ($\sin^2\theta_{23} -
\sin^2\overline{\theta}_{23}$), the statistical significance to exclude CPT
invariance depends strongly on the true value of
$\theta_{23}(\overline{\theta}_{23})$. In case of maximal mixing of
$\theta_{23}$, the CPT conservation will be excluded at 3$\sigma$ C. L. or more
if the difference in the best-fit values of $\theta_{23}$ and
$\overline{\theta}_{23}$ remains as the true.
Searching for neutrinos from solar flares across solar cycles 23 and 24
with the Super-Kamiokande detector
2210.12948 [abs] [pdf]
[abstract]
by K. Okamoto, [and 244 more]K. Abe, Y. Hayato, K. Hiraide, K. Hosokawa, K. Ieki, M. Ikeda, J. Kameda, Y. Kanemura, Y. Kaneshima, Y. Kataoka, Y. Kashiwagi, S. Miki, S. Mine, M. Miura, S. Moriyama, Y. Nagao, M. Nakahata, Y. Nakano, S. Nakayama, Y. Noguchi, K. Sato, H. Sekiya, K. Shimizu, M. Shiozawa, H. Shiba, Y. Sonoda, Y. Suzuki, A. Takeda, Y. Takemoto, A. Takenaka, H. Tanaka, S. Watanabe, T. Yano, S. Han, T. Kajita, K. Okumura, T. Tashiro, T. Tomiya, X. Wang, J. Xia, S. Yoshida, G. D. Megias, P. Fernandez, L. Labarga, N. Ospina, B. Zaldivar, B. W. Pointon, E. Kearns, J. L. Raaf, L. Wan, T. Wester, J. Bian, N. J. Griskevich, W. R. Kropp, S. Locke, M. B. Smy, H. W. Sobel, V. Takhistov, A. Yankelevich, J. Hill, J. Y. Kim, S. H. Lee, I. T. Lim, D. H. Moon, R. G. Park, B. Bodur, K. Scholberg, C. W. Walter, A. Beauchene, L. Bernard, A. Coffani, O. Drapier, S. El Hedri, A. Giampaolo, Th. A. Mueller, A. D. Santos, P. Paganini, B. Quilain, T. Ishizuka, T. Nakamura, J. S. Jang, J. G. Learned, K. Choi, S. Cao, L. H. V. Anthony, D. Martin, M. Scott, A. A. Sztuc, Y. Uchida, V. Berardi, M. G. Catanesi, E. Radicioni, N. F. Calabria, L. N. Machado, G. De Rosa, G. Collazuol, F. Iacob, M. Lamoureux, M. Mattiazzi, L. Ludovici, M. Gonin, G. Pronost, C. Fujisawa, Y. Maekawa, Y. Nishimura, M. Friend, T. Hasegawa, T. Ishida, T. Kobayashi, M. Jakkapu, T. Matsubara, T. Nakadaira, K. Nakamura, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, N. Bhuiyan, T. Boschi, G. T. Burton, F. Di Lodovico, J. Gao, A. Goldsack, T. Katori, J. Migenda, M. Taani, Z. Xie, S. Zsoldos, Y. Kotsar, H. Ozaki, A. T. Suzuki, Y. Takeuchi, S. Yamamoto, C. Bronner, J. Feng, T. Kikawa, M. Mori, T. Nakaya, R. A. Wendell, K. Yasutome, S. J. Jenkins, N. McCauley, P. Mehta, A. Tarrant, K. M. Tsui, Y. Fukuda, Y. Itow, H. Menjo, K. Ninomiya, J. Lagoda, S. M. Lakshmi, M. Mandal, P. Mijakowski, Y. S. Prabhu, J. Zalipska, M. Jia, J. Jiang, C. K. Jung, C. Vilela, M. J. Wilking, C. Yanagisawa, M. Harada, H. Ishino, S. Ito, H. Kitagawa, Y. Koshio, W. Ma, F. Nakanishi, N. Piplani, S. Sakai, G. Barr, D. Barrow, L. Cook, S. Samani, D. Wark, A. Holin, F. Nova, J. Y. Yang, J. E. P. Fannon, M. Malek, J. M. McElwee, O. Stone, M. D. Thiesse, L. F. Thompson, H. Okazawa, S. B. Kim, E. Kwon, J. W. Seo, I. Yu, A. K. Ichikawa, K. D. Nakamura, S. Tairafune, K. Nishijima, M. Koshiba, K. Iwamoto, K. Nakagiri, Y. Nakajima, S. Shima, N. Taniuchi, M. Yokoyama, K. Martens, P. de Perio, M. R. Vagins, M. Kuze, S. Izumiyama, M. Inomoto, M. Ishitsuka, H. Ito, T. Kinoshita, R. Matsumoto, Y. Ommura, N. Shigeta, M. Shinoki, T. Suganuma, K. Yamauchi, J. F. Martin, H. A. Tanaka, T. Towstego, R. Akutsu, R. Gaur, V. Gousy-Leblanc, M. Hartz, A. Konaka, X. Li, N. W. Prouse, S. Chen, B. D. Xu, B. Zhang, M. Posiadala-Zezula, S. B. Boyd, D. Hadley, M. Nicholson, M. O'Flaherty, B. Richards, A. Ali, B. Jamieson, J. Walker, Ll. Marti, A. Minamino, G. Pintaudi, S. Sano, R. Sasaki, S. Suzuki, and K. Wada [hide authors].
Neutrinos associated with solar flares (solar-flare neutrinos) provide
information on particle acceleration mechanisms during the impulsive phase of
solar flares. We searched using the Super-Kamiokande detector for neutrinos
from solar flares that occurred during solar cycles $23$ and $24$, including
the largest solar flare (X28.0) on November 4th, 2003. In order to minimize the
background rate we searched for neutrino interactions within narrow time
windows coincident with $\gamma$-rays and soft X-rays recorded by satellites.
In addition, we performed the first attempt to search for solar-flare neutrinos
from solar flares on the invisible side of the Sun by using the emission time
of coronal mass ejections (CMEs). By selecting twenty powerful solar flares
above X5.0 on the visible side and eight CMEs whose emission speed exceeds
$2000$ $\mathrm{km \, s^{-1}}$ on the invisible side from 1996 to 2018, we
found two (six) neutrino events coincident with solar flares occurring on the
visible (invisible) side of the Sun, with a typical background rate of $0.10$
($0.62$) events per flare in the MeV-GeV energy range. No significant
solar-flare neutrino signal above the estimated background rate was observed.
As a result we set the following upper limit on neutrino fluence at the Earth
$\mathit{\Phi}<1.1\times10^{6}$ $\mathrm{cm^{-2}}$ at the $90\%$ confidence
level for the largest solar flare. The resulting fluence limits allow us to
constrain some of the theoretical models for solar-flare neutrino emission.
Uncovering the neutrino mass ordering with the next galactic
core-collapse supernova neutrino burst using water Cherenkov detectors
2210.11676 [abs] [pdf]
[abstract]
by César Jesús-Valls.
A major conundrum of particle physics is what mass ordering (MO) follow
neutrinos. Due to matter effects the flavor content of the neutrino flux from a
Core-Collapse Supernovae (CCSNe) is expected to be highly dependent on the true
neutrino MO. In this article, the potential to uncover the true neutrino MO
using CCSN neutrinos and water Cherenkov detectors is studied. A novel analysis
strategy is presented, designed to be robust to all existing systematic
uncertainties and readily applicable to the Super-Kamiokande or
Hyper-Kamiokande experiments. The results show that for a paradigmatic CCSN at
10~kpc, Hyper-Kamiokande might discriminate the true neutrino MO with a
confidence similar to 2-3~$\sigma$. In the case of a nearby CCSN at a radius of
3.5~kpc (1~kpc) from Earth, Hyper-Kamiokande (Super-Kamiokande) would reach a
sensitivity beyond 5~$\sigma$.
A lab scale experiment for keV sterile neutrino search
2210.11108 [abs] [pdf]
[abstract]
by Y. C. Lee, [and 9 more]H. B. Kim, H. L. Kim, S. K. Kim, Y. H. Kim, D. H. Kwon, H. S. Lim, H. S. Park, K. R. Woo, and Y. S. Yoon [hide authors].
We developed a simple small-scale experiment to measure the beta decay
spectrum of $^{3}$H. The aim of this research is to investigate the presence of
sterile neutrinos in the keV region. Tritium nuclei were embedded in a
1$\times$1$\times$1 cm$^3$ LiF crystal from the $^6$Li(n,$\alpha$)$^3$H
reaction. The energy of the beta electrons absorbed in the LiF crystal was
measured with a magnetic microcalorimeter at 40 mK. We report a new method of
sample preparation, experiments, and analysis of $^3$H beta measurements. The
spectrum of a 10-hour measurement agrees well with the expected spectrum of
$^3$H beta decay. The analysis results indicate that this method can be used to
search for keV-scale sterile neutrinos.
First constraints on light sterile neutrino oscillations from combined
appearance and disappearance searches with the MicroBooNE detector
2210.10216 [abs] [pdf]
[abstract]
by MicroBooNE collaboration, [and 186 more]P. Abratenko, D. Andrade Aldana, J. Anthony, L. Arellano, J. Asaadi, A. Ashkenazi, S. Balasubramanian, B. Baller, G. Barr, J. Barrow, V. Basque, L. Bathe-Peters, O. Benevides Rodrigues, S. Berkman, A. Bhanderi, M. Bhattacharya, M. Bishai, A. Blake, B. Bogart, T. Bolton, J. Y. Book, L. Camilleri, D. Caratelli, I. Caro Terrazas, F. Cavanna, G. Cerati, Y. Chen, J. M. Conrad, M. Convery, L. Cooper-Troendle, J. I. Crespo-Anadon, M. Del Tutto, S. R. Dennis, P. Detje, A. Devitt, R. Diurba, R. Dorrill, K. Duffy, S. Dytman, B. Eberly, A. Ereditato, J. J. Evans, R. Fine, O. G. Finnerud, B. T. Fleming, N. Foppiani, W. Foreman, D. Franco, A. P. Furmanski, D. Garcia-Gamez, S. Gardiner, G. Ge, S. Gollapinni, O. Goodwin, E. Gramellini, P. Green, H. Greenlee, W. Gu, R. Guenette, P. Guzowski, L. Hagaman, O. Hen, R. Hicks, C. Hilgenberg, G. A. Horton-Smith, B. Irwin, R. Itay, C. James, X. Ji, L. Jiang, J. H. Jo, R. A. Johnson, Y. J. Jwa, D. Kalra, N. Kamp, G. Karagiorgi, W. Ketchum, M. Kirby, T. Kobilarcik, I. Kreslo, M. B. Leibovitch, I. Lepetic, J. -Y. Li, K. Li, Y. Li, K. Lin, B. R. Littlejohn, W. C. Louis, X. Luo, K. Manivannan, C. Mariani, D. Marsden, J. Marshall, N. Martinez, D. A. Martinez Caicedo, K. Mason, A. Mastbaum, N. McConkey, V. Meddage, K. Miller, J. Mills, K. Mistry, T. Mohayai, A. Mogan, M. Mooney, A. F. Moor, C. D. Moore, L. Mora Lepin, J. Mousseau, S. Mulleria Babu, D. Naples, A. Navrer-Agasson, N. Nayak, M. Nebot-Guinot, J. Nowak, M. Nunes, N. Oza, O. Palamara, N. Pallat, V. Paolone, A. Papadopoulou, V. Papavassiliou, H. Parkinson, S. F. Pate, N. Patel, Z. Pavlovic, E. Piasetzky, I. Ponce-Pinto, I. Pophale, S. Prince, X. Qian, J. L. Raaf, V. Radeka, M. Reggiani-Guzzo, L. Ren, L. Rochester, J. Rodriguez Rondon, M. Rosenberg, M. Ross-Lonergan, C. Rudolph von Rohr, G. Scanavini, D. W. Schmitz, A. Schukraft, W. Seligman, M. H. Shaevitz, R. Sharankova, J. Shi, A. Smith, E. L. Snider, M. Soderberg, S. Soldner-Rembold, J. Spitz, M. Stancari, J. St. John, T. Strauss, S. Sword-Fehlberg, A. M. Szelc, W. Tang, N. Taniuchi, K. Terao, C. Thorpe, D. Torbunov, D. Totani, M. Toups, Y. -T. Tsai, J. Tyler, M. A. Uchida, T. Usher, B. Viren, M. Weber, H. Wei, A. J. White, Z. Williams, S. Wolbers, T. Wongjirad, M. Wospakrik, K. Wresilo, N. Wright, W. Wu, E. Yandel, T. Yang, L. E. Yates, H. W. Yu, G. P. Zeller, J. Zennamo, and C. Zhang [hide authors].
We present a search for eV-scale sterile neutrino oscillations in the
MicroBooNE liquid argon detector, simultaneously considering all possible
appearance and disappearance effects within the $3+1$ active-to-sterile
neutrino oscillation framework. We analyze the neutrino candidate events for
the recent measurements of charged-current $\nu_e$ and $\nu_{\mu}$ interactions
in the MicroBooNE detector, using data corresponding to an exposure of
6.37$\times$10$^{20}$ protons on target from the Fermilab booster neutrino
beam. We observe no evidence of light sterile neutrino oscillations and derive
exclusion contours at the $95\%$ confidence level in the plane of the
mass-squared splitting $\Delta m^2_{41}$ and the sterile neutrino mixing angles
$\theta_{\mu e}$ and $\theta_{ee}$, excluding part of the parameter space
allowed by experimental anomalies. Cancellation of $\nu_e$ appearance and
$\nu_e$ disappearance effects due to the full $3+1$ treatment of the analysis
leads to a degeneracy when determining the oscillation parameters, which is
discussed in this paper and will be addressed by future analyses.
Symmetry in neutrino oscillation in matter: New picture and the $ν$SM
-- non-unitarity interplay
2210.09453 [abs] [pdf]
[abstract]
by Hisakazu Minakata.
We update and summarize the present status of our understanding of the
reparametrization symmetry with $i \leftrightarrow j$ state exchange in
neutrino oscillation in matter. We introduce a systematic method called
``Symmetry Finder'' (SF) to uncover such symmetries, demonstrate its efficient
hunting capability, and examine their characteristic features. Apparently they
have a local nature: The 1-2 and 1-3 state exchange symmetries exist at around
the solar- and atmospheric-resonances, respectively, with the level-crossing
states exchanged. However, this view is not supported, to date, in the globally
valid Denton et al. (DMP) perturbation theory, which possesses the 1-2 exchange
symmetry but not the 1-3. It is probably due to lack of our understanding, and
we find a clue for a larger symmetry structure than that we know. In the latter
part of this article, we introduce non-unitarity, or unitarity violation (UV),
into the $\nu$SM neutrino paradigm, a low-energy description of beyond $\nu$SM
new physics at high (or low) scale. Based on the analyses of UV extended
versions of the atmospheric-resonance and the DMP perturbation theories, we
argue that the reparametrization symmetry has a diagnostics capability for the
theory with the $\nu$SM and UV sectors. A speculation is given on the
topological nature of the identity which determines the transformation property
of the UV $\alpha$ parameters.
Expected geoneutrino signal at JUNO using local integrated 3-D refined
crustal model
2210.09165 [abs] [pdf]
[abstract]
by Ran Han, [and 13 more]ZhiWei Li, Ruohan Gao, Yao Sun, Ya Xu, Yaping Cheng, Guangzheng Jiang, Jie Pang, Fengcheng Liu, Andong Wang, Yufei Xi, Liangjian Wen, Jun Cao, and Yu-Feng Li [hide authors].
Geoneutrinos are a unique tool that brings to the surface information about
our planet, in particular, its radiogenic power, insights formation and
chemical composition. To date, only the KamLAND and Borexino experiments
observed geoneutrino, with the former characterized by low concentration of
heat-producing elements in the Earth in contrast to the latter that sets tight
upper limits on the power of a georeactor hypothesized. With respect to the
results yielded therefrom, a small discrepancy has been identified. On this
account, next generation experiments like JUNO are needed if it is to provide
definitive results with respect to the Earth's radiogenic power, and to fully
exploit geoneutrinos to better understand deep Earth.
An accurate a priori prediction of the crustal contribution plays an
important role in enabling the translation of a particle physics measurement
into geo-scientific questions. The existing GIGJ model of JUNO only focused on
constructing a geophysical model of the local crust, without local geochemical
data. Another existing JULOC includes both data, but only able to be achieved
for the top layer of the upper crust, not in deep vertical. This paper reports
on the development of JUNO's first 3-D integrated model, JULOC-I, which
combines seismic, gravity, rock sample and thermal flow data with new building
method, solved the problem in vertical depth.
JULOC-I results show higher than expected geoneutrino signals are mainly
attributable to higher U and Th in southern China than that found elsewhere on
Earth. Moreover, the high level of accuracy of the JULOC-I model, complemented
by 10 years of experimental data, indicates that JUNO has an opportunity to
test different mantle models. Predictions by JULOC-I can be tested after JUNO
goes online and higher accuracy local crustal model continue to play an
important role to improve mantle measurements precision.
Effect of Matter Density in T2HK and DUNE
2210.09103 [abs] [pdf]
[abstract]
by Monojit Ghosh and Osamu Yasuda.
CP phase determination for the near future long baseline experiments, T2HK
and DUNE, will require precise measurements of the oscillation probabilities.
However, the uncertainty in the Earth's density must be considered in
determining these oscillation probabilities. Therefore, in this study, we
update the individual sensitivities of these experiments for determining the
current unknowns in the standard three flavor scenario considering the latest
configuration and also the complementarity between them while considering the
uncertainty in the density. Our study showed that this uncertainty has a
non-negligible impact on the precision of the CP phase determination
particularly for DUNE.
Model Independent Approach of the JUNO $^8$B Solar Neutrino Program
2210.08437 [abs] [pdf]
[abstract]
by JUNO Collaboration, [and 603 more]Jie Zhao, Baobiao Yue, Haoqi Lu, Yufeng Li, Jiajie Ling, Zeyuan Yu, Angel Abusleme, Thomas Adam, Shakeel Ahmad, Rizwan Ahmed, Sebastiano Aiello, Muhammad Akram, Abid Aleem, Tsagkarakis Alexandros, Fengpeng An, Qi An, Giuseppe Andronico, Nikolay Anfimov, Vito Antonelli, Tatiana Antoshkina, Burin Asavapibhop, João Pedro Athayde Marcondes de André, Didier Auguste, Weidong Bai, Nikita Balashov, Wander Baldini, Andrea Barresi, Davide Basilico, Eric Baussan, Marco Bellato, Antonio Bergnoli, Thilo Birkenfeld, Sylvie Blin, David Blum, Simon Blyth, Anastasia Bolshakova, Mathieu Bongrand, Clément Bordereau, Dominique Breton, Augusto Brigatti, Riccardo Brugnera, Riccardo Bruno, Antonio Budano, Jose Busto, Ilya Butorov, Anatael Cabrera, Barbara Caccianiga, Hao Cai, Xiao Cai, Yanke Cai, Zhiyan Cai, Riccardo Callegari, Antonio Cammi, Agustin Campeny, Chuanya Cao, Guofu Cao, Jun Cao, Rossella Caruso, Cédric Cerna, Chi Chan, Jinfan Chang, Yun Chang, Guoming Chen, Pingping Chen, Po-An Chen, Shaomin Chen, Xurong Chen, Yixue Chen, Yu Chen, Zhiyuan Chen, Zikang Chen, Jie Cheng, Yaping Cheng, Alexander Chepurnov, Alexey Chetverikov, Davide Chiesa, Pietro Chimenti, Artem Chukanov, Gérard Claverie, Catia Clementi, Barbara Clerbaux, Marta Colomer Molla, Selma Conforti Di Lorenzo, Daniele Corti, Flavio Dal Corso, Olivia Dalager, Christophe De La Taille, Zhi Deng, Ziyan Deng, Wilfried Depnering, Marco Diaz, Xuefeng Ding, Yayun Ding, Bayu Dirgantara, Sergey Dmitrievsky, Tadeas Dohnal, Dmitry Dolzhikov, Georgy Donchenko, Jianmeng Dong, Evgeny Doroshkevich, Marcos Dracos, Frédéric Druillole, Ran Du, Shuxian Du, Stefano Dusini, Martin Dvorak, Timo Enqvist, Heike Enzmann, Andrea Fabbri, Donghua Fan, Lei Fan, Jian Fang, Wenxing Fang, Marco Fargetta, Dmitry Fedoseev, Zhengyong Fei, Li-Cheng Feng, Qichun Feng, Richard Ford, Amélie Fournier, Haonan Gan, Feng Gao, Alberto Garfagnini, Arsenii Gavrikov, Marco Giammarchi, Nunzio Giudice, Maxim Gonchar, Guanghua Gong, Hui Gong, Yuri Gornushkin, Alexandre Göttel, Marco Grassi, Maxim Gromov, Vasily Gromov, Minghao Gu, Xiaofei Gu, Yu Gu, Mengyun Guan, Yuduo Guan, Nunzio Guardone, Cong Guo, Jingyuan Guo, Wanlei Guo, Xinheng Guo, Yuhang Guo, Paul Hackspacher, Caren Hagner, Ran Han, Yang Han, Miao He, Wei He, Tobias Heinz, Patrick Hellmuth, Yuekun Heng, Rafael Herrera, YuenKeung Hor, Shaojing Hou, Yee Hsiung, Bei-Zhen Hu, Hang Hu, Jianrun Hu, Jun Hu, Shouyang Hu, Tao Hu, Yuxiang Hu, Zhuojun Hu, Guihong Huang, Hanxiong Huang, Kaixuan Huang, Wenhao Huang, Xin Huang, Xingtao Huang, Yongbo Huang, Jiaqi Hui, Lei Huo, Wenju Huo, Cédric Huss, Safeer Hussain, Ara Ioannisian, Roberto Isocrate, Beatrice Jelmini, Ignacio Jeria, Xiaolu Ji, Huihui Jia, Junji Jia, Siyu Jian, Di Jiang, Wei Jiang, Xiaoshan Jiang, Xiaoping Jing, Cécile Jollet, Leonidas Kalousis, Philipp Kampmann, Li Kang, Rebin Karaparambil, Narine Kazarian, Amina Khatun, Khanchai Khosonthongkee, Denis Korablev, Konstantin Kouzakov, Alexey Krasnoperov, Nikolay Kutovskiy, Pasi Kuusiniemi, Tobias Lachenmaier, Cecilia Landini, Sébastien Leblanc, Victor Lebrin, Frederic Lefevre, Ruiting Lei, Rupert Leitner, Jason Leung, Daozheng Li, Demin Li, Fei Li, Fule Li, Gaosong Li, Huiling Li, Mengzhao Li, Min Li, Nan Li, Nan Li, Qingjiang Li, Ruhui Li, Rui Li, Shanfeng Li, Tao Li, Teng Li, Weidong Li, Weiguo Li, Xiaomei Li, Xiaonan Li, Xinglong Li, Yi Li, Yichen Li, Zepeng Li, Zhaohan Li, Zhibing Li, Ziyuan Li, Zonghai Li, Hao Liang, Hao Liang, Jiajun Liao, Ayut Limphirat, Guey-Lin Lin, Shengxin Lin, Tao Lin, Ivano Lippi, Fang Liu, Haidong Liu, Haotian Liu, Hongbang Liu, Hongjuan Liu, Hongtao Liu, Hui Liu, Jianglai Liu, Jinchang Liu, Min Liu, Qian Liu, Qin Liu, Runxuan Liu, Shubin Liu, Shulin Liu, Xiaowei Liu, Xiwen Liu, Yan Liu, Yunzhe Liu, Alexey Lokhov, Paolo Lombardi, Claudio Lombardo, Kai Loo, Chuan Lu, Jingbin Lu, Junguang Lu, Shuxiang Lu, Bayarto Lubsandorzhiev, Sultim Lubsandorzhiev, Livia Ludhova, Arslan Lukanov, Daibin Luo, Fengjiao Luo, Guang Luo, Shu Luo, Wuming Luo, Xiaojie Luo, Vladimir Lyashuk, Bangzheng Ma, Bing Ma, Qiumei Ma, Si Ma, Xiaoyan Ma, Xubo Ma, Jihane Maalmi, Jingyu Mai, Yury Malyshkin, Roberto Carlos Mandujano, Fabio Mantovani, Francesco Manzali, Xin Mao, Yajun Mao, Stefano M. Mari, Filippo Marini, Cristina Martellini, Gisele Martin-Chassard, Agnese Martini, Matthias Mayer, Davit Mayilyan, Ints Mednieks, Yue Meng, Anselmo Meregaglia, Emanuela Meroni, David Meyhöfer, Mauro Mezzetto, Jonathan Miller, Lino Miramonti, Paolo Montini, Michele Montuschi, Axel Müller, Massimiliano Nastasi, Dmitry V. Naumov, Elena Naumova, Diana Navas-Nicolas, Igor Nemchenok, Minh Thuan Nguyen Thi, Alexey Nikolaev, Feipeng Ning, Zhe Ning, Hiroshi Nunokawa, Lothar Oberauer, Juan Pedro Ochoa-Ricoux, Alexander Olshevskiy, Domizia Orestano, Fausto Ortica, Rainer Othegraven, Alessandro Paoloni, Sergio Parmeggiano, Yatian Pei, Nicomede Pelliccia, Anguo Peng, Haiping Peng, Yu Peng, Zhaoyuan Peng, Frédéric Perrot, Pierre-Alexandre Petitjean, Fabrizio Petrucci, Oliver Pilarczyk, Luis Felipe Piñeres Rico, Artyom Popov, Pascal Poussot, Ezio Previtali, Fazhi Qi, Ming Qi, Sen Qian, Xiaohui Qian, Zhen Qian, Hao Qiao, Zhonghua Qin, Shoukang Qiu, Gioacchino Ranucci, Neill Raper, Alessandra Re, Henning Rebber, Abdel Rebii, Mariia Redchuk, Mariia Redchuk, Bin Ren, Jie Ren, Barbara Ricci, Mariam Rifai, Mathieu Roche, Narongkiat Rodphai, Aldo Romani, Bedřich Roskovec, Xichao Ruan, Arseniy Rybnikov, Andrey Sadovsky, Paolo Saggese, Simone Sanfilippo, Anut Sangka, Utane Sawangwit, Julia Sawatzki, Michaela Schever, Cédric Schwab, Konstantin Schweizer, Alexandr Selyunin, Andrea Serafini, Giulio Settanta, Mariangela Settimo, Zhuang Shao, Vladislav Sharov, Arina Shaydurova, Jingyan Shi, Yanan Shi, Vitaly Shutov, Andrey Sidorenkov, Fedor Šimkovic, Chiara Sirignano, Jaruchit Siripak, Monica Sisti, Maciej Slupecki, Mikhail Smirnov, Oleg Smirnov, Thiago Sogo-Bezerra, Sergey Sokolov, Julanan Songwadhana, Boonrucksar Soonthornthum, Albert Sotnikov, Ondřej Šrámek, Warintorn Sreethawong, Achim Stahl, Luca Stanco, Konstantin Stankevich, Dušan Štefánik, Hans Steiger, Jochen Steinmann, Tobias Sterr, Matthias Raphael Stock, Virginia Strati, Alexander Studenikin, Jun Su, Shifeng Sun, Xilei Sun, Yongjie Sun, Yongzhao Sun, Zhengyang Sun, Narumon Suwonjandee, Michal Szelezniak, Jian Tang, Qiang Tang, Quan Tang, Xiao Tang, Alexander Tietzsch, Igor Tkachev, Tomas Tmej, Marco Danilo Claudio Torri, Konstantin Treskov, Andrea Triossi, Giancarlo Troni, Wladyslaw Trzaska, Cristina Tuve, Nikita Ushakov, Vadim Vedin, Giuseppe Verde, Maxim Vialkov, Benoit Viaud, Cornelius Moritz Vollbrecht, Cristina Volpe, Katharina von Sturm, Vit Vorobel, Dmitriy Voronin, Lucia Votano, Pablo Walker, Caishen Wang, Chung-Hsiang Wang, En Wang, Guoli Wang, Jian Wang, Jun Wang, Lu Wang, Meifen Wang, Meng Wang, Meng Wang, Ruiguang Wang, Siguang Wang, Wei Wang, Wei Wang, Wenshuai Wang, Xi Wang, Xiangyue Wang, Yangfu Wang, Yaoguang Wang, Yi Wang, Yi Wang, Yifang Wang, Yuanqing Wang, Yuman Wang, Zhe Wang, Zheng Wang, Zhimin Wang, Zongyi Wang, Apimook Watcharangkool, Wei Wei, Wei Wei, Wenlu Wei, Yadong Wei, Kaile Wen, Liangjian Wen, Christopher Wiebusch, Steven Chan-Fai Wong, Bjoern Wonsak, Diru Wu, Qun Wu, Zhi Wu, Michael Wurm, Jacques Wurtz, Christian Wysotzki, Yufei Xi, Dongmei Xia, Xiang Xiao, Xiaochuan Xie, Yuguang Xie, Zhangquan Xie, Zhao Xin, Zhizhong Xing, Benda Xu, Cheng Xu, Donglian Xu, Fanrong Xu, Hangkun Xu, Jilei Xu, Jing Xu, Meihang Xu, Yin Xu, Yu Xu, Baojun Yan, Taylor Yan, Wenqi Yan, Xiongbo Yan, Yupeng Yan, Changgen Yang, Chengfeng Yang, Huan Yang, Jie Yang, Lei Yang, Xiaoyu Yang, Yifan Yang, Yifan Yang, Haifeng Yao, Jiaxuan Ye, Mei Ye, Ziping Ye, Frédéric Yermia, Na Yin, Zhengyun You, Boxiang Yu, Chiye Yu, Chunxu Yu, Hongzhao Yu, Miao Yu, Xianghui Yu, Zezhong Yu, Cenxi Yuan, Chengzhuo Yuan, Ying Yuan, Zhenxiong Yuan, Noman Zafar, Vitalii Zavadskyi, Shan Zeng, Tingxuan Zeng, Yuda Zeng, Liang Zhan, Aiqiang Zhang, Bin Zhang, Binting Zhang, Feiyang Zhang, Guoqing Zhang, Honghao Zhang, Jialiang Zhang, Jiawen Zhang, Jie Zhang, Jin Zhang, Jingbo Zhang, Jinnan Zhang, Mohan Zhang, Peng Zhang, Qingmin Zhang, Shiqi Zhang, Shu Zhang, Tao Zhang, Xiaomei Zhang, Xin Zhang, Xuantong Zhang, Xueyao Zhang, Yinhong Zhang, Yiyu Zhang, Yongpeng Zhang, Yu Zhang, Yuanyuan Zhang, Yumei Zhang, Zhenyu Zhang, Zhijian Zhang, Fengyi Zhao, Rong Zhao, Runze Zhao, Shujun Zhao, Dongqin Zheng, Hua Zheng, Yangheng Zheng, Weirong Zhong, Jing Zhou, Li Zhou, Nan Zhou, Shun Zhou, Tong Zhou, Xiang Zhou, Jiang Zhu, Jingsen Zhu, Kangfu Zhu, Kejun Zhu, Zhihang Zhu, Bo Zhuang, Honglin Zhuang, Liang Zong, and Jiaheng Zou [hide authors].
The physics potential of detecting $^8$B solar neutrinos is exploited at the
Jiangmen Underground Neutrino Observatory (JUNO), in a model independent manner
by using three distinct channels of the charged-current (CC), neutral-current
(NC) and elastic scattering (ES) interactions. Due to the largest-ever mass of
$^{13}$C nuclei in the liquid-scintillator detectors and the potential low
background level, $^8$B solar neutrinos would be observable in the CC and NC
interactions on $^{13}$C for the first time. By virtue of optimized event
selections and muon veto strategies, backgrounds from the accidental
coincidence, muon-induced isotopes, and external backgrounds can be greatly
suppressed. Excellent signal-to-background ratios can be achieved in the CC, NC
and ES channels to guarantee the $^8$B solar neutrino observation. From the
sensitivity studies performed in this work, we show that one can reach the
precision levels of 5%, 8% and 20% for the $^8$B neutrino flux,
$\sin^2\theta_{12}$, and $\Delta m^2_{21}$, respectively, using ten years of
JUNO data. It would be unique and helpful to probe the details of both solar
physics and neutrino physics. In addition, when combined with SNO, the
world-best precision of 3% is expected for the $^8$B neutrino flux measurement.
Interpreting Reactor Antineutrino Anomalies with STEREO data
2210.07664 [abs] [pdf]
[abstract]
by H. Almazán, [and 23 more]L. Bernard, A. Blanchet, A. Bonhomme, C. Buck, A. Chalil, P. del Amo Sanchez, I. El Atmani, L. Labit, J. Lamblin A. Letourneau D. Lhuillier, M. Licciardi, M. Lindner, T. Materna, H. Pessard, J. -S. Réal, J. -S. Ricol, C. Roca, R. Rogly, T. Salagnac, V. Savu, S. Schoppmann, T. Soldner, A. Stutz, and M. Vialat [hide authors].
Anomalies in past neutrino measurements have led to the discovery that these
particles have non-zero mass and oscillate between their three flavors when
they propagate. In the 2010's, similar anomalies observed in the antineutrino
spectra emitted by nuclear reactors have triggered the hypothesis of the
existence of a supplementary neutrino state that would be sterile i.e. not
interacting via the weak interaction. The STEREO experiment was designed to
study this scientific case that would potentially extend the Standard Model of
Particle Physics. Here we present a complete study based on our full set of
data with significantly improved sensitivity. Installed at the ILL (Institut
Laue Langevin) research reactor, STEREO has accurately measured the
antineutrino energy spectrum associated to the fission of 235U. This
measurement confirms the anomalies whereas, thanks to the segmentation of the
STEREO detector and its very short mean distance to the core (10~m), the same
data reject the hypothesis of a light sterile neutrino. Such a direct
measurement of the antineutrino energy spectrum suggests instead that biases in
the nuclear experimental data used for the predictions are at the origin of the
anomalies. Our result supports the neutrino content of the Standard Model and
establishes a new reference for the 235U antineutrino energy spectrum. We
anticipate that this result will allow to progress towards finer tests of the
fundamental properties of neutrinos but also to benchmark models and nuclear
data of interest for reactor physics and for observations of astrophysical or
geo-neutrinos.
Impact of the finite life-time of UHECR sources
2210.07090 [abs] [pdf]
[abstract]
by Björn Eichmann and Michael Kachelrieß.
The observational data on ultrahigh energy cosmic rays (UHECR), in particular
their mass composition, show strong indications for extremely hard spectra of
individual mass groups of CR nuclei at Earth. In this work, we show that such
hard spectra can be the result of the finite life-time of UHECR sources, if a
few individual sources dominate the UHECR flux at the highest energies. In this
case, time delays induced by deflections in the turbulent extragalactic
magnetic field as well as from the diffusive or advective escape from the
source environment can suppress low-energy CRs, leading to a steepening of the
observed spectrum. Considering radio galaxies as the main source of UHECRs, we
discuss the necessary conditions that few individual sources dominate over the
total contribution from the bulk of sources that have been active in the past.
We provide two proof-of-principle scenarios showing that for a turbulent
extragalactic magnetic field with a strength $B$ and a coherence length $l_{\rm
coh}$, the life-time of a source at a distance $d_{\rm src}$ should satisfy
${t_{\rm act} \sim \left( B/1\,\text{nG} \right)^2\,\left( d_{\rm
src}/10\,\text{Mpc} \right)^2\,\left( l_{\rm coh}/1\,\text{Mpc}
\right)\,\text{Myr}}$ to obtain the necessary hardening of the CR spectrum at
Earth.
Evidence of a signature of planet formation processes from solar
neutrino fluxes
2210.06900 [abs] [pdf]
[abstract]
by Masanobu Kunitomo, Tristan Guillot, and Gaël Buldgen.
Solar evolutionary models are thus far unable to reproduce spectroscopic,
helioseismic, and neutrino constraints consistently, resulting in the so-called
solar modeling problem. In parallel, planet formation models predict that the
evolving composition of the protosolar disk and, thus, of the gas accreted by
the proto-Sun must have been variable. We show that solar evolutionary models
that include a realistic planet formation scenario lead to an increased core
metallicity of up to 5%, implying that accurate neutrino flux measurements are
sensitive to the initial stages of the formation of the Solar System. Models
with homogeneous accretion match neutrino constraints to no better than
2.7$\sigma$. In contrast, accretion with a variable composition due to planet
formation processes, leading to metal-poor accretion of the last $\sim$4% of
the young Sun's total mass, yields solar models within 1.3$\sigma$ of all
neutrino constraints. We thus demonstrate that in addition to increased
opacities at the base of the convective envelope, the formation history of the
Solar System constitutes a key element in resolving the current crisis of solar
models.
Astrophysical searches of ultralight particles
2210.06837 [abs] [pdf]
[abstract]
by Tanmay Kumar Poddar.
The Standard Model of particle physics is a $SU(3)_c\times SU(2)_L\times
U(1)_Y$ gauge theory that can explain the strong, weak, and electromagnetic
interactions between the particles. The gravitational interaction is described
by Einstein's General Relativity theory which is a classical theory of gravity.
These theories can explain all the four fundamental forces of nature with great
level of accuracy. However, there are several theoretical and experimental
motivations of studying physics beyond the Standard Model of particle physics
and Einstein's General Relativity theory. Probing these new physics scenarios
with ultralight particles has its own importance as they can be a promising
candidates for dark matter that can evade the constraints from dark matter
direct detection experiments and solve the small scale structure problems of
the universe. In this paper, we have considered axions and gauge bosons as
light particles and their possible searches through astrophysical observations.
In particular, we obtain constraints on ultralight axions from orbital period
loss of compact binary systems, gravitational light bending, and Shapiro time
delay. We also derive constraints on ultralight gauge bosons from indirect
evidence of gravitational waves, and perihelion precession of planets. Such
type of observations can also constrain several particle physics models and are
discussed.
Lorentz invariance violation induced threshold anomaly versus very-high
energy cosmic photon emission from GRB 221009A
2210.06338 [abs] [pdf]
[abstract]
by Hao Li and Bo-Qiang Ma.
It has been reported that the Large High Altitude Air Shower Observatory
(LHAASO) observed very high energy photons from GRB 221009A, with the highest
energy reaching 18~TeV. We find that observation of such high energy photons is
quite nontrivial since extragalactic background light could absorb these
photons severely and the flux is too weak to be observed. Therefore we discuss
a potential mechanism for us to observe these photons, and suggest that Lorentz
invariance violation induced threshold anomaly of the process \(\gamma\gamma\to
e^-e^+\) provides a candidate to explain this phenomenon.
Constraints on populations of neutrino sources from searches in the
directions of IceCube neutrino alerts
2210.04930 [abs] [pdf]
[abstract]
by R. Abbasi, [and 383 more]M. Ackermann, J. Adams, N. Aggarwal, J. A. Aguilar, M. Ahlers, J. M. Alameddine, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, V. Basu, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. Benda, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Y. Book, J. Borowka, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Braun, B. Brinson, J. Brostean-Kaiser, R. T. Burley, R. S. Busse, M. A. Campana, E. G. Carnie-Bronca, C. Chen, Z. Chen, D. Chirkin, K. Choi, B. A. Clark, L. Classen, A. Coleman, G. H. Collin, A. Connolly, J. M. Conrad, P. Coppin, P. Correa, S. Countryman, D. F. Cowen, R. Cross, C. Dappen, P. Dave, C. De Clercq, J. J. DeLaunay, D. Delgado López, H. Dembinski, K. Deoskar, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, H. Dujmovic, M. A. DuVernois, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, K. L. Fan, A. R. Fazely, A. Fedynitch, N. Feigl, S. Fiedlschuster, A. T. Fienberg, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, A. Garcia, S. Garrappa, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glauch, T. Glüsenkamp, N. Goehlke, J. G. Gonzalez, S. Goswami, D. Grant, S. J. Gray, T. Grégoire, S. Griswold, C. Günther, P. Gutjahr, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, H. Hamdaoui, M. Ha Minh, K. Hanson, J. Hardin, A. A. Harnisch, P. Hatch, A. Haungs, K. Helbing, J. Hellrung, F. Henningsen, L. Heuermann, S. Hickford, A. Hidvegi, C. Hill, G. C. Hill, K. D. Hoffman, K. Hoshina, W. Hou, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, K. Hymon, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, M. Jin, B. J. P. Jones, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, L. Kardum, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, J. L. Kelley, A. Kheirandish, K. Kin, J. Kiryluk, S. R. Klein, A. Kochocki, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, T. Kozynets, E. Krupczak, E. Kun, N. Kurahashi, N. Lad, C. Lagunas Gualda, M. J. Larson, F. Lauber, J. P. Lazar, J. W. Lee, K. Leonard, A. Leszczyńska, M. Lincetto, Q. R. Liu, M. Liubarska, E. Lohfink, C. Love, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, S. Mancina, W. Marie Sainte, I. C. Mariş, S. Marka, Z. Marka, M. Marsee, I. Martinez-Soler, R. Maruyama, T. McElroy, F. McNally, J. V. Mead, K. Meagher, S. Mechbal, A. Medina, M. Meier, S. Meighen-Berger, Y. Merckx, J. Micallef, D. Mockler, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, T. Mukherjee, R. Naab, R. Nagai, U. Naumann, A. Nayerhoda, J. Necker, M. Neumann, H. Niederhausen, M. U. Nisa, A. Noell, S. C. Nowicki, A. Obertacke Pollmann, M. Oehler, B. Oeyen, A. Olivas, R. Orsoe, J. Osborn, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, L. Paul, C. Pérez de los Heros, L. Peters, J. Peterson, S. Philippen, S. Pieper, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, B. Pries, R. Procter-Murphy, G. T. Przybylski, C. Raab, J. Rack-Helleis, M. Rameez, K. Rawlins, Z. Rechav, A. Rehman, P. Reichherzer, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, E. J. Roberts, S. Robertson, S. Rodan, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, L. Ruohan, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, J. Saffer, D. Salazar-Gallegos, P. Sampathkumar, S. E. Sanchez Herrera, A. Sandrock, M. Santander, S. Sarkar, S. Sarkar, J. Savelberg, M. Schaufel, H. Schieler, S. Schindler, B. Schlueter, T. Schmidt, J. Schneider, F. G. Schröder, L. Schumacher, G. Schwefer, S. Sclafani, S. Seunarine, A. Sharma, S. Shefali, N. Shimizu, M. Silva, B. Skrzypek, B. Smithers, R. Snihur, J. Soedingrekso, A. Søgaard, D. Soldin, C. Spannfellner, G. M. Spiczak, C. Spiering, M. Stamatikos, T. Stanev, R. Stein, T. Stezelberger, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, S. Ter-Antonyan, W. G. Thompson, J. Thwaites, S. Tilav, K. Tollefson, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, C. F. Tung, R. Turcotte, J. P. Twagirayezu, B. Ty, M. A. Unland Elorrieta, K. Upshaw, N. Valtonen-Mattila, J. Vandenbroucke, N. van Eijndhoven, D. Vannerom, J. van Santen, J. Vara, J. Veitch-Michaelis, S. Verpoest, D. Veske, C. Walck, W. Wang, T. B. Watson, C. Weaver, P. Weigel, A. Weindl, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. H. Wiebusch, N. Willey, D. R. Williams, M. Wolf, G. Wrede, J. Wulff, X. W. Xu, J. P. Yanez, E. Yildizci, S. Yoshida, S. Yu, T. Yuan, Z. Zhang, and P. Zhelnin [hide authors].
Beginning in 2016, the IceCube Neutrino Observatory has sent out alerts in
real time containing the information of high-energy ($E \gtrsim 100$~TeV)
neutrino candidate events with moderate-to-high ($\gtrsim 30$\%) probability of
astrophysical origin. In this work, we use a recent catalog of such alert
events, which, in addition to events announced in real-time, includes events
that were identified retroactively, and covers the time period of 2011-2020. We
also search for additional, lower-energy, neutrinos from the arrival directions
of these IceCube alerts. We show how performing such an analysis can constrain
the contribution of rare populations of cosmic neutrino sources to the diffuse
astrophysical neutrino flux. After searching for neutrino emission coincident
with these alert events on various timescales, we find no significant evidence
of either minute-scale or day-scale transient neutrino emission or of steady
neutrino emission in the direction of these alert events. This study also shows
how numerous a population of neutrino sources has to be to account for the
complete astrophysical neutrino flux. Assuming sources have the same
luminosity, an $E^{-2.5}$ neutrino spectrum and number densities that follow
star-formation rates, the population of sources has to be more numerous than
$7\times 10^{-9}~\textrm{Mpc}^{-3}$. This number changes to $3\times
10^{-7}~\textrm{Mpc}^{-3}$ if number densities instead have no cosmic
evolution.
Directional Neutrino Searches for Galactic Center Dark Matter at Large
Underground LArTPCs
2210.04920 [abs] [pdf]
[abstract]
by Matthew R. Buckley, Andrew Mastbaum, and Gopolang Mohlabeng.
We investigate the sensitivity of a large, underground LArTPC-based neutrino
detector to dark matter in the Galactic Center annihilating into neutrinos.
Such a detector could have the ability to resolve the direction of the electron
in a neutrino scattering event, and thus to infer information about the source
direction for individual neutrino events. We consider the improvements on the
expected experimental sensitivity that this directional information would
provide. Even without directional information, we find a DUNE-like LArTPC
detector is capable of setting limits on dark matter annihilation to neutrinos
for dark matter masses above 30 MeV that are competitive with or exceed current
experimental reach. While currently-demonstrated angular resolution for
low-energy electrons is insufficient to allow any significant increase in
sensitivity, these techniques could benefit from improvements to algorithms and
the additional spatial information provided by novel 3D charge imaging
approaches. We consider the impact of such enhancements to the resolution for
electron directionality, and find that where electron-scattering events can be
distinguished from charged-current neutrino interactions, limits on dark matter
annihilation in the mass range where solar neutrino backgrounds dominate
($\lesssim 15$ MeV) can be significantly improved using directional
information, and would be competitive with existing limits using $40$
kton$\times$year of exposure.
Monoenergetic Neutrinos from WIMP Annihilation in Jupiter
2210.04761 [abs] [pdf]
[abstract]
by George M. French and Marc Sher.
Weakly interacting massive particles (WIMPs) can be captured by the Sun and
annihilate in the core, which may result in production of kaons that can decay
at rest into monoenergetic 236 MeV neutrinos. Several studies of detection of
these neutrinos at DUNE have been carried out. It has been shown that if the
WIMP mass is below 4 GeV, then they will evaporate prior to annihilation,
suppressing the signal. Since Jupiter has a cooler core, WIMPs with masses in
the 1-4 GeV range will not evaporate and can thus annihilate into monoenergetic
neutrinos. We calculate the flux of these neutrinos near the surface of Jupiter
and find that it is comparable to the flux at DUNE for masses above 4 GeV and
substantially greater in the 1-4 GeV range. Of course, detecting these
neutrinos would require a neutrino detector near Jupiter. Obviously, it will be
many decades before such a detector can be built, but should direct detection
experiments find a WIMP with a mass in the 1-4 GeV range, it may be one of the
few ways to learn about the annihilation process. A liquid hydrogen time
projection chamber might be able to get precise directional information and
energy of these neutrinos (and hydrogen is plentiful in the vicinity of
Jupiter). We speculate that such a detector could be placed on the far side of
one of the tidally locked Amalthean moons; the moon itself would provide
substantial background shielding and the surface would allow easier deployment
of solar panels for power generation.
The impact of neutrino-nucleus interaction modeling on new physics
searches
2210.03753 [abs] [pdf]
[abstract]
by Nina M. Coyle, Shirley Weishi Li, and Pedro A. N. Machado.
Accurate neutrino-nucleus interaction modeling is an essential requirement
for the success of the accelerator-based neutrino program. As no satisfactory
description of cross sections exists, experiments tune neutrino-nucleus
interactions to data to mitigate mis-modeling. In this work, we study how the
interplay between near detector tuning and cross section mis-modeling affects
new physics searches. We perform a realistic simulation of neutrino events and
closely follow NOvA's tuning, the first published of such procedures in a
neutrino experiment. We analyze two illustrative new physics scenarios, sterile
neutrinos and light neutrinophilic scalars, presenting the relevant
experimental signatures and the sensitivity regions with and without tuning.
While the tuning does not wash out sterile neutrino oscillation patterns, cross
section mis-modeling can bias the experimental sensitivity. In the case of
light neutrinophilic scalars, variations in cross section models completely
dominate the sensitivity regardless of any tuning. Our findings reveal the
critical need to improve our theoretical understanding of neutrino-nucleus
interactions, and to estimate the impact of tuning on new physics searches. We
urge neutrino experiments to follow NOvA's example and publish the details of
their tuning procedure, and to develop strategies to more robustly account for
cross section uncertainties, which will expand the scope of their physics
program.
New Constraints on Dark Matter and Cosmic Neutrino Profiles through
Gravity
2210.03749 [abs] [pdf]
[abstract]
by Yu-Dai Tsai, [and 4 more]Joshua Eby, Jason Arakawa, Davide Farnocchia, and Marianna S. Safronova [hide authors].
We derive purely gravitational constraints on dark matter and cosmic neutrino
profiles in the solar system using asteroid (101955) Bennu. We focus on Bennu
because of its extensive tracking data and high-fidelity trajectory modeling
resulting from the OSIRIS-REx mission. We find that the local density of dark
matter is bound by $\rho_{\rm DM}\lesssim 3.3\times 10^{-15}\;\rm kg/m^3 \simeq
6\times10^6\,\bar{\rho}_{\rm DM}$, in the vicinity of $\sim 1.1$ au (where
$\bar{\rho}_{\rm DM}\simeq 0.3\;\rm GeV/cm^3$). We show that high-precision
tracking data of solar system objects can constrain cosmic neutrino
overdensities relative to the Standard Model prediction $\bar{n}_{\nu}$, at the
level of $\eta\equiv n_\nu/\bar{n}_{\nu}\lesssim 1.7 \times 10^{11}(0.1 \;{\rm
eV}/m_\nu)$ (Saturn), comparable to the existing bounds from KATRIN and other
previous laboratory experiments (with $m_\nu$ the neutrino mass). These local
bounds have interesting implications for existing and future direct-detection
experiments. Our constraints apply to all dark matter candidates but are
particularly meaningful for scenarios including solar halos, stellar basins,
and axion miniclusters, which predict or allow overdensities in the solar
system. Furthermore, introducing a DM-SM long-range fifth force with a strength
$\tilde{\alpha}_D$ times stronger than gravity, Bennu can set a constraint on
$\rho_{\rm DM}\lesssim \bar{\rho}_{\rm DM}\left(6 \times
10^6/\tilde{\alpha}_D\right)$. These constraints can be improved in the future
as the accuracy of tracking data improves, observational arcs increase, and
more missions visit asteroids.
Decay of superluminal neutrinos in the collinear approximation
2210.02222 [abs] [pdf]
[abstract]
by J. M. Carmona, [and 3 more]J. L. Cortés, J. J. Relancio, and M. A. Reyes [hide authors].
The kinematics of the three body decay, with a modified energy-momentum
relation of the particles due to a violation of Lorentz invariance, is
presented in detail in the collinear approximation. The results are applied to
the decay of superluminal neutrinos producing an electron-positron or a
neutrino-antineutrino pair. Explicit expressions for the energy distributions,
required for a study of the cascade of neutrinos produced in the propagation of
superluminal neutrinos, are derived.
High-energy neutrino-induced cascade from the direction of the flaring
radio blazar TXS 0506+056 observed by the Baikal Gigaton Volume Detector in
2021
2210.01650 [abs] [pdf]
[abstract]
by Baikal-GVD Collaboration, [and 10 more]A. K. Erkenov, N. A. Kosogorov, Y. A. Kovalev, Y. Y. Kovalev, A. V. Plavin, A. V. Popkov, A. B. Pushkarev, D. V. Semikoz, Y. V. Sotnikova, and S. V. Troitsky [hide authors].
The existence of high-energy astrophysical neutrinos has been unambiguously
demonstrated, but their sources remain elusive. IceCube reported an association
of a 290-TeV neutrino with a gamma-ray flare of TXS 0506+056, an active
galactic nucleus with a compact radio jet pointing to us. Later, radio blazars
were shown to be associated with IceCube neutrino events with high statistical
significance. These associations remained unconfirmed with the data of
independent experiments. Here we report on the detection of a rare neutrino
event with the estimated energy of 224 +- 75 TeV from the direction of TXS
0506+056 by the new Baikal-GVD neutrino telescope in April 2021 followed by a
radio flare observed by RATAN-600. This event is the highest-energy cascade
detected so far by Baikal-GVD from a direction below horizon. The result
supports previous suggestions that radio blazars in general, and TXS 0506+056
in particular, are the sources of high-energy neutrinos, and opens up the
cascade channel for the neutrino astronomy.
Solar and supernova neutrino physics with future NaI(Tl) dark matter
search detectors
2210.01386 [abs] [pdf]
[abstract]
by Young Ju Ko and Hyun Su Lee.
We investigate the prospects for measuring the coherent elastic
neutrino-nucleus scattering of solar and supernova neutrinos in future NaI(Tl)
dark matter detection experiments. Considering the reduced background and
improved light yield of the recently developed NaI(Tl) crystals, more than
3$\sigma$ observation sensitivities of the supernova neutrino within the Milky
Way are demonstrated. In the case of the solar neutrino, approximately 3
observations are marginal with a 1 ton NaI(Tl) experiment assuming an order of
magnitude reduced background, five photoelectron thresholds, and 5-year data
exposure.
Dark Matter decay to neutrinos
2210.01303 [abs] [pdf]
[abstract]
by Carlos A. Argüelles, [and 6 more]Diyaselis Delgado, Avi Friedlander, Ali Kheirandish, Ibrahim Safa, Aaron C. Vincent, and Henry White [hide authors].
It is possible that the strongest interactions between dark matter and the
Standard Model occur via the neutrino sector. Unlike gamma rays and charged
particles, neutrinos provide a unique avenue to probe for astrophysical sources
of dark matter, since they arrive unimpeded and undeflected from their sources.
Previously, we reported on annihilations of dark matter to neutrinos; here, we
review constraints on the decay of dark matter into neutrinos over a range of
dark matter masses from MeV to ZeV, compiling previously reported limits,
exploring new electroweak corrections and computing constraints where none have
been computed before. We examine the expected contributions to the neutrino
flux at current and upcoming neutrino experiments as well as photons from
electroweak emission expected at gamma-ray telescopes, leading to constraints
on the dark matter decay lifetime, which ranges from $\tau \sim
1.2\times10^{21}$ s at 10 MeV to $1.5\times10^{29}$s at 1 PeV.
September 2022
How to Identify Different New Neutrino Oscillation Physics Scenarios at
DUNE
2210.00109 [abs] [pdf]
[abstract]
by Peter B. Denton, Alessio Giarnetti, and Davide Meloni.
Next generation neutrino oscillation experiments are expected to measure the
remaining oscillation parameters with very good precision. They will have
unprecedented capabilities to search for new physics that modify oscillations.
DUNE, with its broad band beam, good particle identification, and relatively
high energies will provide an excellent environment to search for new physics.
If deviations from the standard three-flavor oscillation picture are seen
however, it is crucial to know which new physics scenario is found so that it
can be verified elsewhere and theoretically understood. We investigate several
benchmark new physics scenarios by looking at existing long-baseline
accelerator neutrino data from NOvA and T2K and determine at what sensitivity
DUNE can differentiate among them. We consider sterile neutrinos and both
vector and scalar non-standard neutrino interactions, all with new complex
phases, the latter of which could conceivably provide absolute neutrino mass
scale information. We find that, in many interesting cases, DUNE will have good
model discrimination. We also perform a new fit to NOvA and T2K data with
scalar NSI.
Neutrino propagation in the Earth and emerging charged leptons with
$\texttt{nuPyProp}$
2209.15581 [abs] [pdf]
[abstract]
by Diksha Garg, [and 24 more]Sameer Patel, Mary Hall Reno, Alexander Reustle, Yosui Akaike, Luis A. Anchordoqui, Douglas R. Bergman, Isaac Buckland, Austin L. Cummings, Johannes Eser, Fred Garcia, Claire Guépin, Tobias Heibges, Andrew Ludwig, John F. Krizmanic, Simon Mackovjak, Eric Mayotte, Sonja Mayotte, Angela V. Olinto, Thomas C. Paul, Andrés Romero-Wolf, Frédéric Sarazin, Tonia M. Venters, Lawrence Wiencke, and Stephanie Wissel [hide authors].
Ultra-high-energy neutrinos serve as messengers of some of the highest energy
astrophysical environments. Given that neutrinos are neutral and only interact
via weak interactions, neutrinos can emerge from sources, traverse astronomical
distances, and point back to their origins. Their weak interactions require
large target volumes for neutrino detection. Using the Earth as a neutrino
converter, terrestrial, sub-orbital, and satellite-based instruments are able
to detect signals of neutrino-induced extensive air showers. In this paper, we
describe the software code $\texttt{nuPyProp}$ that simulates tau neutrino and
muon neutrino interactions in the Earth and predicts the spectrum of the
$\tau$-lepton and muons that emerge. The $\texttt{nuPyProp}$ outputs are lookup
tables of charged lepton exit probabilities and energies that can be used
directly or as inputs to the $\texttt{nuSpaceSim}$ code designed to simulate
optical and radio signals from extensive air showers induced by the emerging
charged leptons. We describe the inputs to the code, demonstrate its
flexibility and show selected results for $\tau$-lepton and muon exit
probabilities and energy distributions. The $\texttt{nuPyProp}$ code is open
source, available on Github.
Solar neutrino physics
2209.14832 [abs] [pdf]
[abstract]
by Xun-Jie Xu, Zhe Wang, and Shaomin Chen.
As a free, intensive, rarely interactive and well directional messenger,
solar neutrinos have been driving both solar physics and neutrino physics
developments for more than half a century. Since more extensive and advanced
neutrino experiments are under construction, being planned or proposed, we are
striving toward an era of precise and comprehensive measurement of solar
neutrinos in the next decades. In this article, we review recent theoretical
and experimental progress achieved in solar neutrino physics. We present not
only an introduction to neutrinos from the standard solar model and the
standard flavor evolution, but also a compilation of a variety of new physics
that could affect and hence be probed by solar neutrinos. After reviewing the
latest techniques and issues involved in the measurement of solar neutrino
spectra and background reduction, we provide our anticipation on the physics
gains from the new generation of neutrino experiments.
The Status of the Galactic Center Gamma-Ray Excess
2209.14370 [abs] [pdf]
[abstract]
by Dan Hooper.
The Galactic Center Gamma-Ray Excess has a spectrum, angular distribution,
and overall intensity that agree remarkably well with that expected from
annihilating dark matter particles in the form of a $m_X \sim 50 \, {\rm GeV}$
thermal relic. Previous claims that these photons are clustered on small
angular scales or trace the distribution of known stellar populations once
appeared to favor interpretations in which this signal originates from a large
population of unresolved millisecond pulsars. More recent work, however, has
overturned these conclusions, finding that the observed gamma-ray excess does
{\it not} contain discernible small scale power, and is distributed with
approximate spherical symmetry, not tracing any known stellar populations. In
light of these results, it now appears significantly more likely that the
Galactic Center Gamma-Ray Excess is produced by annihilating dark matter.
Non-standard neutrino interactions in light mediator models at reactor
experiments
2209.13566 [abs] [pdf]
[abstract]
by Bhaskar Dutta, [and 4 more]Sumit Ghosh, Tianjun Li, Adrian Thompson, and Ankur Verma [hide authors].
Compared to other neutrino sources, the huge anti-neutrino fluxes at nuclear
reactor based experiments empower us to derive stronger bounds on non-standard
interactions of neutrinos with electrons mediated by light scalar/vector
mediators. At neutrino energy around $200$~keV reactor anti-neutrino flux is at
least an order of magnitude larger compared to the solar flux. The atomic and
crystal form factors of the detector materials related to the details of the
atomic structure becomes relevant at this energy scale as the momentum
transfers would be small. Non-standard neutrino-electron interaction mediated
by light scalar/vector mediator arises naturally in many low-scale models. We
also propose one such new model with a light scalar mediator. Here, we
investigate the parameter space of such low-scale models in reactor based
neutrino experiments with low threshold Ge and Si detectors, and find the
prospect of probing/ruling out the relevant parameter space by finding the
projected sensitivity at $90 \%$ confidence level by performing a
$\chi^2$-analysis. We find that a detector capable of discriminating between
electron recoil and nuclear recoil signal down to a very low threshold such as
$5$~eV placed in reactor based experiment would be able to probe a larger
region in parameter space compared to the previously explored region. A Ge (Si)
detector with $10$~kg-yr exposure and 1 MW reactor anti-neutrino flux would be
able to probe the scalar and vector mediators with masses below 1 keV for
coupling products $\sqrt{g_\nu g_e}$ $\sim$ $1 \times 10^{-6}~(9.5 \times
10^{-7})$ and $1\times 10^{-7} ~(8\times 10^{-8})$, respectively.
Neutrino non-radiative decay and the diffuse supernova neutrino
background
2209.12465 [abs] [pdf]
[abstract]
by Pilar Ivanez-Ballesteros and M. Cristina Volpe.
We revisit the possibility that neutrinos undergo non-radiative decay. We
investigate the potential to extract information on the neutrino
lifetime-to-mass ratio from the diffuse supernova neutrino background. To this
aim, we explicitly consider the current uncertainties on the core-collapse
supernova rate and the fraction of failed supernovae. We present predictions in
a full 3 neutrino framework in the absence and presence of neutrino
non-radiative decay, for the Super-Kamiokande+Gd, the JUNO, the
Hyper-Kamiokande, and the DUNE experiments, that should observe the diffuse
supernova neutrino background in the near future. Our results show the
importance of a 3 neutrino treatment of neutrino decay and of identifying the
neutrino mass ordering to break possible degeneracies between DSNB predictions
in the presence of decay and standard physics.
Strong Supernova 1987A Constraints on Bosons Decaying to Neutrinos
2209.11773 [abs] [pdf]
[abstract]
by Damiano F. G. Fiorillo, Georg G. Raffelt, and Edoardo Vitagliano.
Majoron-like bosons would emerge from a supernova (SN) core by neutrino
coalescence of the form $\nu\nu\to\phi$ and $\bar\nu\bar\nu\to\phi$ with 100
MeV-range energies. Subsequent decays to (anti)neutrinos of all flavors provide
a flux component with energies much larger than the usual flux from the
``neutrino sphere.'' The absence of 100 MeV-range events in the Kamiokande~II
and IMB signal of SN~1987A implies that less than 1\% of the total energy was
thus emitted and provides the strongest constraint on the majoron-neutrino
coupling of $g\lesssim 10^{-9}\,{\rm MeV}/m_\phi$ for $100~{\rm eV}\lesssim
m_\phi\lesssim 100~{\rm MeV}$. It is straightforward to extend our new argument
to other hypothetical feebly interacting particles.
Determination of the total cross section and $ρ$-parameter from
elastic scattering in $pp$ collisions at $\sqrt{s}=13$ TeV with the ATLAS
detector
2209.11487 [abs] [pdf]
[abstract]
by Hasko Stenzel.
A new measurement of elastic $pp$ scattering at $\sqrt{s} = 13$ TeV with the
ATLAS-ALFA detector is presented. The measurement was performed using data
recorded in a special run of the LHC with $\beta^\star = 2.5$ km. The elastic
cross-section was measured differentially in the Mandelstam $t$ variable and
from a fit to ${\textrm{d}}\sigma/\textrm{d}t$ the total cross section, the
$\rho$-parameter and parameters of the nuclear slope are determined. The
results for $\sigma_{\textrm{tot}}$ and $\rho$ are \begin{equation*}
\sigma_{\textrm{tot}}(pp\rightarrow X) = \mbox{104.7} \; \pm 1.1 \; \mbox{mb} ,
\; \; \rho = \mbox{0.098} \; \pm 0.011 . \end{equation*} The energy evolution
of $\sigma_{\textrm{tot}}$ and $\rho$, connected through dispersion relations,
is compared to several models. Furthermore, the total inelastic cross section
is determined from the difference of the total and elastic cross section, and
the ratio of the elastic to total cross section is calculated.
Probing non-unitarity of neutrino mixing in the scenario of Lorentz
violation and dark nonstandard interaction
2209.10233 [abs] [pdf]
[abstract]
by Trisha Sarkar.
Neutrino flavour oscillation is one of the primary indication of the
existence of new physics beyond standard model. The presence of small neutrino
mass is indispensable to explicate the oscillation among different flavours of
neutrino. By the addition of a right handed neutral lepton with the standard
model fermions, it is possible to generate tiny neutrino mass. Such additional
fermion may induce non-unitarity to the $3\times 3$ PMNS mixing matrix which
influences the propagation of neutrino in space-time. In this work the effect
of non-unitary mixing matrix is analyzed in neutrino oscillation in presence of
two new physics scenarios, Lorentz violation and dark non-standard interaction.
Lorentz symmetry violation mainly appears at the Planck scale, which may also
be manifested at a lower energy level. On the other hand, dark non standard
interaction arises due to the interaction of neutrino with the environmental
dark matter which contributes as a perturbative correction to the neutrino
mass. In this analysis, the comparative study of unitary and non-unitary mixing
matrix is carried out considering the scenario of Lorentz violation and dark
NSI in the context of long baseline DUNE and short baseline Daya Bay
experimental set up. The signature of dark nonstandard interaction is
observable in both DUNE and Daya Bay set up in terms of large value of neutrino
survival and oscillation probability respectively and is a possible explanation
for the excess flux observed at $\sim5$ MeV in Daya Bay experiment. The
signature of Lorentz violation is also possible to be observed in the short
baseline Daya Bay experiment only.
Prospects for detection of a Galactic diffuse neutrino flux
2209.10011 [abs] [pdf]
[abstract]
by Pedro De la Torre Luque, Daniele Gaggero, and Dario Grasso.
A Galactic cosmic-ray transport model featuring non-homogeneous transport has
been developed over the latest years. This setup is aimed at reproducing
gamma-ray observations in different regions of the Galaxy (with particular
focus on the progressive hardening of the hadronic spectrum in the inner
Galaxy) and was shown to be compatible with the very-high-energy gamma-ray
diffuse emission recently detected up to PeV energies. In this work, we extend
the results previously presented to test the reliability of that model
throughout the whole sky. To this aim, we compare our predictions with detailed
longitude and latitude profiles of the diffuse gamma-ray emission measured by
Fermi-LAT for different energies and compute the expected Galactic neutrino
diffuse emission, comparing it with current limits from the ANTARES
collaboration. We emphasize that the possible detection of a Galactic neutrino
component will allow us to break the degeneracy between our model and other
scenarios featuring prominent contributions from unresolved sources and TeV
halos.
Floating Dark Matter in Celestial Bodies
2209.09834 [abs] [pdf]
[abstract]
by Rebecca K. Leane and Juri Smirnov.
Dark matter (DM) can be captured in celestial bodies after scattering and
losing sufficient energy to become gravitationally bound. We derive a general
framework that describes the current DM distribution inside celestial objects,
which self-consistently includes the effects of concentration diffusion,
thermal diffusion, gravity, and capture accumulation. For DM with sufficient
interactions, we show that a significant DM population can thermalize and sit
towards the celestial-body surface. This floating distribution allows for new
phenomenology for DM searches in a wide range of celestial bodies, including
the Sun, Earth, Jupiter, Brown Dwarfs, and Exoplanets.
Neutrino forces in neutrino backgrounds
2209.07082 [abs] [pdf]
[abstract]
by Mitrajyoti Ghosh, [and 4 more]Yuval Grossman, Walter Tangarife, Xun-Jie Xu, and Bingrong Yu [hide authors].
The Standard Model predicts a long-range force, proportional to $G_F^2/r^5$,
between fermions due to the exchange of a pair of neutrinos. This quantum force
is feeble and has not been observed yet. In this paper, we compute this force
in the presence of neutrino backgrounds, both for isotropic and directional
background neutrinos. We find that for the case of directional background the
force can have a $1/r$ dependence and it can be significantly enhanced compared
to the vacuum case. In particular, background effects caused by reactor, solar,
and supernova neutrinos enhance the force by many orders of magnitude. The
enhancement, however, occurs only in the direction parallel to the direction of
the background neutrinos. We discuss the experimental prospects of detecting
the neutrino force in neutrino backgrounds and find that the effect is close to
the available sensitivity of the current fifth force experiments. Yet, the
angular spread of the neutrino flux and that of the test masses reduce the
strength of this force. The results are encouraging and a detailed experimental
study is called for to check if the effect can be probed.
New constraints on the dark matter-neutrino and dark matter-photon
scattering cross sections from TXS 0506+056
2209.06339 [abs] [pdf]
[abstract]
by Francesc Ferrer, Gonzalo Herrera, and Alejandro Ibarra.
The flux of high energy neutrinos and photons produced in a blazar could get
attenuated when they propagate through the dark matter spike around the central
black hole and the halo of the host galaxy. Using the observation by IceCube of
a few high-energy neutrino events from TXS 0506+056, and their coincident gamma
ray events, we obtain new constraints on the dark matter-neutrino and dark
matter-photon scattering cross sections. Our constraints are orders of
magnitude more stringent than those derived from considering the attenuation
through the intergalactic medium and the Milky Way dark matter halo. When the
cross-section increases with energy, our constraints are also stronger than
those derived from the CMB and large-scale structure.
Probing Quantum Gravity with Elastic Interactions of Ultra-High-Energy
Neutrinos
2209.06282 [abs] [pdf]
[abstract]
by Alfonso Garcia Soto, [and 3 more]Diksha Garg, Mary Hall Reno, and Carlos A. Argüelles [hide authors].
The next generation of radio telescopes will be sensitive to low-scale
quantum gravity by measuring ultra-high-energy neutrinos. In this letter, we
demonstrate for the first time that neutrino-nucleon soft interactions induced
by TeV-scale gravity would significantly increase the number of events detected
by the IceCube-Gen2 radio array in the EeV regime. However, we show that these
experiments cannot measure the total cross section using only the angular and
energy information of the neutrino flux, unless assumptions on the underlying
inelasticity distribution of neutral interactions are made.
Imprints of scalar NSI on the CP-violation sensitivity using synergy
among DUNE, T2HK and T2HKK
2209.05287 [abs] [pdf]
[abstract]
by Abinash Medhi, Moon Moon Devi, and Debajyoti Dutta.
The Non-Standard Interactions (NSIs) are subdominant effects, often appearing
in various extensions of SM, which may impact the neutrino oscillations through
matter. It is important and interesting to explore the impact of NSIs in the
ongoing and upcoming precise neutrino oscillations experiments. In this work,
we have studied the imprints of a scalar-mediated NSI in three upcoming
long-baseline (LBL) experiments (DUNE, T2HK, T2HKK). The effects of scalar NSI
appears as a medium-dependent correction to the neutrino mass term. Its
contribution scales linearly with matter density, making LBL experiments a
suitable candidate to probe its effects. We show that the scalar NSI may
significantly impact the oscillation probabilities, event rates at the
detectors and the $\chi^2$-sensitivities of $\delta_{CP}$ measurements. We
present the results of a combined analysis involving the LBL experiments
(DUNE+T2HK, DUNE+T2HKK, DUNE+T2HK+T2HKK) which offer a better capability of
constraining the scalar NSI parameters as well as an improved sensitivity
towards CP-violation.
Majorana versus Dirac Constraints on the Neutrino Dipole Moments
2209.03373 [abs] [pdf]
[abstract]
by André de Gouvêa, [and 3 more]Giancarlo Jusino Sánchez, Pedro A. N. Machado, and Zahra Tabrizi [hide authors].
Massive neutrinos are guaranteed to have nonzero electromagnetic moments and,
since there are at least three neutrino species, these dipole moments define a
matrix. Here, we estimate the current upper bounds on all independent neutrino
electromagnetic moments, concentrating on Earth-bound experiments and
measurements with solar neutrinos, including the very recent results reported
by XENONnT. We make no simplifying assumptions and compare the hypotheses that
neutrinos are Majorana fermions or Dirac fermions. In particular, we fully
explore constraints in the Dirac-neutrino parameter space. Majorana and Dirac
neutrinos are different; for example, the upper bounds on the magnitudes of the
elements of the dipole moment matrix are weaker for Dirac neutrinos, relative
to Majorana neutrinos. The potential physics reach of next-generation
experiments also depends on the nature of the neutrino. We find that a
next-generation experiment two orders of magnitude more sensitive to the
neutrino electromagnetic moments via $\nu_{\mu}$ elastic scattering may
discover that the neutrino electromagnetic moments are nonzero if the neutrinos
are Dirac fermions. Instead, if the neutrinos are Majorana fermions, such a
discovery is ruled out by existing solar neutrino data, unless there are more
than three light neutrinos.
Testing the Gallium Anomaly
2209.02885 [abs] [pdf]
[abstract]
by Patrick Huber.
We study the online detection by gallium capture of mono-energetic neutrinos
produced by a $^{51}$Cr radioactive source in a scintillation experiment. We
find that cerium-doped gadolinium aluminum gallium garnet (GAGG) is a suitable
scintillator which contains about 21% of gallium per weight and has a high mass
density and light yield. Combined with a highly efficient light detection
system this allows tagging of the subsequent germanium decay and thus a clean
distinction of gallium capture and elastic neutrino electron scattering events.
With 1.5 tons of scintillator and 10 source runs of 3.4MCi, each, we obtain
about 760 gallium capture events with a purity of 85% and 680,000 neutrino
electron scattering events, where the latter provide a precise normalization
independent of any nuclear physics. This configuration would allow to test the
gallium anomaly at more than $5\sigma$ in an independent way.
Blazar constraints on neutrino-dark matter scattering
2209.02713 [abs] [pdf]
[abstract]
by James M. Cline, [and 7 more]Shan Gao, Fangyi Guo, Zhongan Lin, Shiyan Liu, Matteo Puel, Phillip Todd, and Tianzhuo Xiao [hide authors].
Neutrino emission in coincidence with gamma rays has been observed from the
blazar TXS 0506+056 by the IceCube telescope. Neutrinos from the blazar had to
pass through a dense spike of dark matter (DM) surrounding the central black
hole. The observation of such a neutrino implies new upper bounds on the
neutrino-DM scattering cross section as a function of DM mass. The constraint
is stronger than existing ones for a range of DM masses, if the cross section
rises linearly with energy. For constant cross sections, competitive bounds are
also possible, depending on details of the DM spike.
Gallium Anomaly: Critical View from the Global Picture of $ν_{e}$ and
$\barν_{e}$ Disappearance
2209.00916 [abs] [pdf]
[abstract]
by C. Giunti, [and 4 more]Y. F. Li, C. A. Ternes, O. Tyagi, and Z. Xin [hide authors].
The significance of the Gallium Anomaly, from the BEST, GALLEX, and SAGE
radioactive source experiments, is quantified using different theoretical
calculations of the neutrino detection cross section, and its explanation due
to neutrino oscillations is compared with the bounds from the analyses of
reactor rate and spectral ratio data, $\beta$-decay data, and solar neutrino
data. In the 3+1 active-sterile neutrino mixing scheme, the Gallium Anomaly is
in strong tension with the individual and combined bounds of these data sets.
In the combined scenario with all available data, the parameter goodness of fit
is below 0.042%, corresponding to a severe tension of 4-5$\sigma$, or stronger.
Therefore, we conclude that one should pursue other possible solutions beyond
short-baseline oscillations for the Gallium Anomaly. We also present a new
global fit of $\nu_e$ and $\bar\nu_e$ disappearance data, showing that there is
a 2.6-3.3$\sigma$ preference in favor of short-baseline oscillations, which is
driven by an updated analysis of reactor spectral ratio data.
Comment on "Damping of neutrino oscillations, decoherence and the
lengths of neutrino wave packets''
2209.00561 [abs] [pdf]
[abstract]
by B. J. P. Jones.
We point out three apparent inconsistencies in the treatment of oscillation
coherence from reactor neutrino and source neutrino experiments in recent paper
"Damping of neutrino oscillations, decoherence and the lengths of neutrino wave
packets''. First, that the dependence of the oscillation probability upon the
subsequent interactions of entangled recoil particles implies causality
violations and in some situations superluminal signaling; second, that
integrating over a non-orthogonal basis for the entangled recoil leads to
unphysical effects; and third, that the question of what interactions serve to
measure the position of the initial state particle remains ambiguous. These
points taken together appear to undermine the claim made therein that the
effects of wave packet separation must be strictly unobservable in reactor and
radioactive source based neutrino experiments.
Characterising Dark Matter-induced neutrino potentials
2209.00442 [abs] [pdf]
[abstract]
by Gabriel M. Salla.
In this paper we explore interactions between neutrinos and Dark Matter. In
particular, we study how the propagation of astrophysical neutrinos can be
modified by computing the most general potential generated by the galactic DM
background. We use on-shell techniques to compute this potential in a
completely model independent way and obtain an expression valid for any Dark
Matter mass and spin. Afterwards, we use this expression to analyse under what
circumstances such potential can be important at the phenomenological level,
and we find that under some assumptions only ultra light scalar Dark Matter
could be of any relevance to oscillation experiments.
August 2022
Addressing the Short-Baseline Neutrino Anomalies with Energy-Dependent
Mixing Parameters
2209.00031 [abs] [pdf]
[abstract]
by K. S. Babu, [and 3 more]Vedran Brdar, André de Gouvêa, and Pedro A. N. Machado [hide authors].
Several neutrino experiments have reported results that are potentially
inconsistent with our current understanding of the lepton sector. A candidate
solution to these so-called short-baseline anomalies is postulating the
existence of new, eV-scale, mostly sterile neutrinos that mix with the active
neutrinos. This hypothesis, however, is strongly disfavored once one considers
all neutrino data, especially those that constrain the disappearance of muon
and electron neutrinos at short-baselines. Here, we show that if the
sterile-active mixing parameters depend on the energy-scales that characterize
neutrino production and detection, the sterile-neutrino hypothesis may provide
a reasonable fit to all neutrino data. The reason for the improved fit is that
the stringent disappearance constraints on the different elements of the
extended neutrino mixing matrix are associated to production and detection
energy scales that are different from those that characterize the anomalous
LSND and MiniBooNE appearance data. We show, via a concrete example, that
secret interactions among the sterile neutrinos can lead to the results of
interest.
Exploiting stellar explosion induced by the QCD phase transition in
large-scale neutrino detectors
2208.14469 [abs] [pdf]
[abstract]
by Tetyana Pitik, [and 3 more]Daniel Heimsoth, Anna M. Suliga, and A. B. Balantekin [hide authors].
The centers of the core-collapse supernovae are one of the densest
environments in the Universe. Under such conditions, it is conceivable that a
first-order phase transition from ordinary nuclear matter to the quark-gluon
plasma occurs. This transition releases a large amount of latent heat that can
drive a supernova explosion and may imprint a sharp signature in the neutrino
signal. We show how this snap feature, if observed at large-scale neutrino
detectors, can set competitive limits on the neutrino masses and assist the
localization of the supernova via triangulation. The 95\%C.L. limit on the
neutrino mass can reach 0.16~eV in Ice-Cube, 0.22~eV in Hyper-Kamiokande, and
0.58~eV in DUNE, for a supernova at a distance of 10 kpc. For the same distance
and in the most optimistic neutrino conversion case, the triangulation method
can constrain the $1\sigma$ angular uncertainty of the supernova localization
within $\sim 0.3^{\circ}-9.0^{\circ}$ in the considered pairs of the detectors,
leading to an improvement up to an order of magnitude with respect to the often
considered in the literature rise time of the neutronization burst.
Physics implications of recent Dresden-II reactor data
2208.13262 [abs] [pdf]
[abstract]
by Anirban Majumdar, [and 3 more]Dimitrios K. Papoulias, Rahul Srivastava, and José W. F. Valle [hide authors].
Prompted by the recent Dresden-II reactor data we examine its implications
for the determination of the weak mixing angle, paying attention to the effect
of the quenching function. We also determine the resulting constraints on the
unitarity of the neutrino mixing matrix, as well as on the most general type of
nonstandard neutral-current neutrino interactions.
Constraining Non-Standard Interactions with Coherent Elastic
Neutrino-Nucleus Scattering at the European Spallation Source
2208.11771 [abs] [pdf]
[abstract]
by Sabya Sachi Chatterjee, [and 3 more]Stéphane Lavignac, O. G. Miranda, and G. Sanchez Garcia [hide authors].
The European Spallation Source (ESS), currently under construction in Sweden,
will provide an intense pulsed neutrino flux allowing for high-statistics
measurements of coherent elastic neutrino-nucleus scattering (CE{\nu}NS) with
advanced nuclear recoil detectors. In this paper, we investigate in detail the
possibility of constraining non-standard neutrino interactions (NSIs) through
such precision CE{\nu}NS measurements at the ESS, considering the different
proposed detection technologies, either alone or in combination. We first study
the sensitivity to neutral-current NSI parameters that each detector can reach
in 3 years of data taking. We then show that operating two detectors
simultaneously can significantly improve the expected sensitivity on
flavor-diagonal NSI parameters. Combining the results of two detectors turns
out to be even more useful when two NSI parameters are assumed to be
nonvanishing at a time. In this case, suitably chosen detector combinations can
reduce the degeneracies between some pairs of NSI parameters to a small region
of the parameter space.
Quantum Gravitational Decoherence in the 3 Neutrino Flavor Scheme
2208.11754 [abs] [pdf]
[abstract]
by Dominik Hellmann, Heinrich Päs, and Erika Rani.
In many theories of quantum gravity quantum fluctuations of spacetime may
serve as an environment for decoherence. Here we study quantum-gravitational
decoherence of high energy astrophysical neutrinos in the presence of fermionic
dark sectors and for a realistic three neutrino scenario. We show how violation
of global symmetries expected to arise in quantum gravitational interactions
provides a possibility to pin down the number of dark matter fermions in the
universe. Furthermore, we predict the expected total neutrino flux and flavor
ratios at experiments depending on the flavor composition at the source.
Probing neutrino interactions and dark radiation with gravitational
waves
2208.11714 [abs] [pdf]
[abstract]
by Marilena Loverde and Zachary J. Weiner.
After their generation, cosmological backgrounds of gravitational waves
propagate nearly freely but for the expansion of the Universe and the
anisotropic stress of free-streaming particles. Primordial signals -- both that
from inflation and the infrared spectrum associated to subhorizon production
mechanisms -- would carry clean information about the cosmological history of
these effects. We study the modulation of the standard damping of gravitational
waves by free-streaming radiation due to the decoupling (or recoupling) of
interactions. We focus on nonstandard neutrino interactions in effect after the
decoupling of weak interactions as well as more general scenarios in the early
Universe involving other light relics. We develop semianalytic results in fully
free-streaming scenarios to provide intuition for numerical results that
incorporate interaction rates with a variety of temerpature dependencies.
Finally, we compute the imprint of neutrino interactions on the $B$-mode
polarization of the cosmic microwave background, and we comment on other means
to infer the presence of such effects at higher frequencies.
Recent results from the TOTEM collaboration and the discovery of the
odderon
2208.10782 [abs] [pdf]
[abstract]
by C. Royon.
We describe the most recent results from the TOTEM collaboration on elastic,
inelastic and total cross sections as well as the odderon discovery by the D0
and TOTEM collaborations.
The carbon footprint of proposed $\rm e^+e^-$ Higgs factories
2208.10466 [abs] [pdf]
[abstract]
by Patrick Janot and Alain Blondel.
The energy consumption of any of the $\rm e^+e^-$ Higgs factory projects that
can credibly operate immediately after the end of LHC, namely three linear
colliders (CLIC, operating at $\sqrt{s}=380$GeV; and ILC and $\rm C^3$,
operating at $\sqrt{s}=250$ GeV) and two circular colliders (CEPC and FCC-ee,
operating at $\sqrt{s}=240$ GeV), will be everything but negligible. Future
Higgs boson studies may therefore have a significant environmental impact. This
note proposes to include the carbon footprint for a given physics performance
as a top-level gauge for the design optimization and, eventually, the choice of
the future facility. The projected footprints per Higgs boson produced,
evaluated using the 2021 carbon emission of available electricity, are found to
vary by a factor 100 depending on the considered Higgs factory project.
Texture of Two Vanishing Subtraces in Neutrino Mass Matrix and Current
Experimental Tests
2208.10344 [abs] [pdf]
[abstract]
by A. Ismael, E. I. Lashin, and N. Chamoun.
We present a full phenomenological and analytical study for the neutrino mass
matrix characterized by two vanishing $2\times2$ subtraces. We update one past
result in light of the recent experimental data. Out of the fifteen possible
textures, we find seven cases can accommodate the experimental data instead of
eight ones in the past study. We also introduce few symmetry realizations for
viable and nonviable textures based on non-abelian ($A_4$ or $S_4$) flavor
symmetry within type II seesaw scenario.
Discovering neutrinoless double-beta decay in the era of precision
neutrino cosmology
2208.09954 [abs] [pdf]
[abstract]
by Manuel Ettengruber, [and 4 more]Matteo Agostini, Allen Caldwell, Philipp Eller, and Oliver Schulz [hide authors].
We evaluate the discovery probability of a combined analysis of proposed
neutrinoless double-beta decay experiments in a scenario with normal ordered
neutrino masses. The discovery probability strongly depends on the value of the
lightest neutrino mass, ranging from zero in case of vanishing masses and up to
80-90\% for values just below the current constraints. We study the discovery
probability in different scenarios, focusing on the exciting prospect in which
cosmological surveys will measure the sum of neutrino masses. Uncertainties in
nuclear matrix element calculations partially compensate each other when data
from different isotopes are available. Although a discovery is not granted, the
theoretical motivations for these searches and the presence of scenarios with
high discovery probability strongly motivates the proposed international,
multi-isotope experimental program.
Zoom in muon survival probability with sterile neutrino for CP and
T-violation
2208.09696 [abs] [pdf]
[abstract]
by Kiran Sharma and Sudhanwa Patra.
We present the approximated analytic expressions for the muon survival
probability in a $3+1$ mixing scenario in the presence of matter effect using
the S-matrix formalism. We find that all the individual terms contributing to
the muon survival probability can significantly reduce to just three
contributions. The leading order contribution comes from the three flavor muon
survival probability followed by the two sub-leading contributions arising from
active-sterile mixing. Furthermore, to more simplify the results we adopt the
well known series expansion relations about mass-hierarchy parameter $\alpha =
\Delta m^2_{21} / \Delta m^2_{31}$ and the mixing angle $\sin \theta_{13}$ in
the vanishing limit of $\alpha^2$. We discuss the relevance of muon survival
probability to probe the CP and T-violation studies coming from the new
physics. We also compare the analytic relation between vacuum and matter
contributions to the muon survival probability at the leading order. Finally,
we comment on the probability behavior at the various long baselines relevant
to understand the atmospheric-neutrino sector and to resolve the existing
mass-hierarchy problem.
Extra dimensions with light and heavy neutral leptons: An application to
CE$ν$NS
2208.09584 [abs] [pdf]
[abstract]
by Amir N. Khan.
We explore the possibility of relating extra dimensions with light and heavy
Dirac-type neutral leptons and develop a framework for testing them in various
laboratory experiments. The Kaluza-Klein modes in the large extra dimension
models of the light neutral leptons could mix with the standard model neutrinos
and produce observable effects in the oscillation experiments. We show that the
chirality flipping up-scattering processes occurring through either neutrino
magnetic dipole moment or the weakly coupled scalar interactions can also
produce heavy Kaluza-Klein modes of the corresponding right-handed neutral
leptons propagating in one or more extra dimensions. However, to conserve the
four-dimensional energy-momentum, their masses must be below the maximum energy
of the neutrinos in the initial state. The appreciable size of extra dimensions
connected with these heavy neutral leptons can thus affect the cross-sections
of these processes. This framework applies to any up-scattering process. Our
work here focuses only on its application to the coherent elastic
neutrino-nucleus scattering process. We derive constraints on the size of extra
dimensions using the COHERENT data in oscillation and up-scattering processes.
For model with one large extra dimension for the light neutral leptons, we
obtain the limits, $R \sim 3 \ \mu$m (NH) and $R \sim 2.5 \ \mu$m (IH), on the
size of extra dimension corresponding to the absolute mass limit, $m_{0} \leq 3
\times 10^{-3}$ eV at 90$\%$ C.L. from the short-baseline oscillations. Using
the up-scattering process for heavy neutral leptons, we obtain new parameter
spaces between the size of extra dimensions and parameters of the dipole or
scalar interactions.
$E_{\mathrm{iso}}$-$E_{\mathrm{p}}$ correlation of gamma ray bursts:
calibration and cosmological applications
2208.09272 [abs] [pdf]
[abstract]
by X. D. Jia, [and 4 more]J. P. Hu, J. Yang, B. B. Zhang, and F. Y. Wang [hide authors].
Gamma-ray bursts (GRBs) are the most explosive phenomena and can be used to
study the expansion of Universe. In this paper, we compile a long GRB sample
for the $E_{\mathrm{iso}}$-$E_{\mathrm{p}}$ correlation from Swift and Fermi
observations. The sample contains 221 long GRBs with redshifts from 0.03 to
8.20. From the analysis of data in different redshift intervals, we find no
statistically significant evidence for the redshift evolution of this
correlation. Then we calibrate the correlation in six sub-samples and use the
calibrated one to constrain cosmological parameters. Employing a piece-wise
approach, we study the redshift evolution of dark energy equation of state
(EOS), and find that the EOS tends to be oscillating at low redshift, but
consistent with $-1$ at high redshift. It hints a dynamical dark energy at
$2\sigma$ confidence level at low redshift.
UHE neutrinos encountering decaying and non-decaying magnetic fields of
compact stars
2208.06644 [abs] [pdf]
[abstract]
by Neetu Raj Singh Chundawat, Arindam Mandal, and Trisha Sarkar.
The phenomena of neutrino spin flavour precession in the presence of an
extraneous magnetic field is a repercussion of neutrino magnetic moment which
is consociated with the physics beyond the standard model of electroweak
interactions. Ultra high energy neutrinos are spawned from a number of sources
in the universe including the highly energetic astrophysical objects such as
active galactic nuclei, blazar or supermassive black holes. When such high
energy neutrinos pass through any compact stellar objects like neutron stars or
white dwarfs, their flux can significantly reduce due to the exorbitant
magnetic field provided by these compact objects. For Dirac neutrinos, such
phenomena occur due to the conversion of neutrinos to their sterile
counterparts. In this work, we consider a neutron star possessing a spatially
varying magnetic field which may or may not decay with time. We find that, for
the non-decaying magnetic field, the flux of high energy Dirac neutrinos
becomes nearly half after passing through the neutron star. The flux is further
enfeebled by $\sim 10\%$ in the presence of muons inside the neutron star. For
decaying magnetic field, the flux reduction is abated by $\sim 5\%$ as compared
to the temporally static magnetic field. In the case of a white dwarf, the
depletion of flux is lesser as compared to the neutron stars.
Ultra-high energy neutrinos from high-redshift electromagnetic cascades
2208.06440 [abs] [pdf]
[abstract]
by AmirFarzan Esmaeili, [and 3 more]Antonio Capanema, Arman Esmaili, and Pasquale Dario Serpico [hide authors].
We study the impact of the muon pair production and double pair production
processes induced by ultra-high energy photons on the cosmic microwave
background. Although the muon pair production cross section is smaller than the
electron pair production one, the associated energy loss length is comparable
or shorter than the latter (followed by inverse Compton in the deep
Klein-Nishina regime) at high-redshift, where the effect of the astrophysical
radio background is expected to be negligible. By performing a simulation
taking into account the details of $e/\gamma$ interactions at high energies, we
show that a significant fraction of the electromagnetic energy injected at
$E\gtrsim 10^{19}\,$eV at redshift $z\gtrsim 5$ is channeled into neutrinos.
The double pair production plays a crucial role in enhancing the multiplicity
of muon production in these electromagnetic cascades. The ultra-high energy
neutrino spectrum, yet to be detected, can in principle harbour information on
ultra-high energy sources in the young universe, either conventional or exotic
ones, with weaker constraints from the diffuse gamma ray flux compared to their
low redshift counterparts.
Implications of first LZ and XENONnT results: A comparative study of
neutrino properties and light mediators
2208.06415 [abs] [pdf]
[abstract]
by ShivaSankar K. A., [and 4 more]Anirban Majumdar, Dimitrios K. Papoulias, Hemant Prajapati, and Rahul Srivastava [hide authors].
Next generation direct dark matter detection experiments are favorable
facilities to probe neutrino properties and light mediators beyond the Standard
Model. We explore the implications of the recent data reported by LUX-ZEPLIN
(LZ) and XENONnT collaborations on electromagnetic neutrino interactions and
neutrino generalized interactions (NGIs). We show that XENONnT places the most
stringent upper limits on the effective and transition neutrino magnetic moment
(of the order of few $\times 10^{-12}~\mu_B$) as well as stringent constraints
to neutrino millicharge (of the order of $\sim 10^{-13}~e$)--competitive to
LZ--and improved by about one order of magnitude in comparison to existing
constraints coming from Borexino and TEXONO. We furthermore explore the XENONnT
and LZ sensitivities to simplified models with light NGIs and find improved
constraints in comparison to those extracted from Borexino-Phase II data.
Evidence for PeV Proton Acceleration from Fermi-LAT Observations of SNR
G106.3+2.7
2208.05457 [abs] [pdf]
[abstract]
by Ke Fang, [and 4 more]Matthew Kerr, Roger Blandford, Henrike Fleischhack, and Eric Charles [hide authors].
The existence of a "knee" at energy ~1 PeV in the cosmic-ray spectrum
suggests the presence of Galactic PeV proton accelerators called "PeVatrons".
Supernova Remnant (SNR) G106.3+2.7 is a prime candidate for one of these. The
recent detection of very high energy (0.1-100 TeV) gamma rays from G106.3+2.7
may be explained either by the decay of neutral pions or inverse Compton
scattering by relativistic electrons. We report an analysis of 12 years of
Fermi-LAT gamma-ray data which shows that the GeV-TeV gamma-ray spectrum is
much harder and requires a different total electron energy than the radio and
X-ray spectra, suggesting it has a distinct, hadronic origin. The non-detection
of gamma rays below 10 GeV implies additional constraints on the relativistic
electron spectrum. A hadronic interpretation of the observed gamma rays is
strongly supported. This observation confirms the long-sought connection
between Galactic PeVatrons and SNRs. Moreover, it suggests that G106.3+2.7
could be the brightest member of a new population of SNRs whose gamma-ray
energy flux peaks at TeV energies. Such a population may contribute to the
cosmic-ray knee and be revealed by future very high energy gamma-ray detectors.
Implications of the QCD dynamics and a Super-Glashow astrophysical
neutrino flux on the description of ultrahigh energy neutrino data
2208.04597 [abs] [pdf]
[abstract]
by Victor P. Goncalves, Diego R. Gratieri, and Alex S. C. Quadros.
The number of events observed in neutrino telescopes depends on the neutrino
fluxes in the Earth, their absorption while crossing the Earth and their
interaction in the detector. In this paper, we investigate the impact of the
QCD dynamics at high energies on the energy dependence of the average
inelasticity and angular dependence of the absorption probability during the
neutrino propagation through the Earth, as well in the determination of the
properties of the incident astrophysical neutrino flux. Moreover, the number of
events at the IceCube and IceCube - Gen2 are estimated considering different
scenarios for the QCD dynamics and assuming the presence of a hypothetical
Super - Glashow flux, which peaks for energies above the Glashow resonance.
Neutrino Decoherence and the Mass Hierarchy in the JUNO Experiment
2208.04277 [abs] [pdf]
[abstract]
by Eric Marzec and Joshua Spitz.
The finite size of a neutrino wavepacket at creation can affect its
oscillation probability. Here, we consider the electron antineutrino wavepacket
and decoherence in the context of the nuclear reactor based experiment JUNO.
Given JUNO's high expected statistics [$\sim$100k IBD events ($\bar{\nu}_e p
\rightarrow e^+ n$)], long baseline ($\sim$53\,km), and excellent energy
resolution [$\sim$$0.03/\sqrt{E_{\mathrm{vis}}~\mathrm{(MeV)}}$], its
sensitivity to the size of the wavepacket is expected to be quite strong.
Unfortunately, this sensitivity may weaken the experiment's ability to measure
the orientation of the neutrino mass hierarchy for currently allowed values of
the wavepacket size. Here, we report both the JUNO experiment's ability to
determine the hierarchy orientation in the presence of a finite wavepacket and
its simultaneous sensitivity to size of the wavepacket and the hierarchy. We
find that wavepacket effects are relevant for the hierarchy determination up to
nearly two orders of magnitude above the current experimental lower limit on
the size, noting that there is no theoretical consensus on the expectation of
this value. We also consider the effect in the context of other aspects of
JUNO's nominal three-neutrino oscillation measurement physics program and the
prospect of future enhancements to sensitivity, including from precise
measurements of $\Delta m^2_{3l}$ and a near detector.
Implications of Recent KATRIN Results for Lower-Limits on Neutrino
Masses
2208.03790 [abs] [pdf]
[abstract]
by Ephraim Fischbach, [and 3 more]Dennis E. Krause, Quan Le Thien, and Carol Scarlett [hide authors].
Recently announced results from the KATRIN collaboration imply an upper bound
on the effective electron anti-neutrino mass $m_{\nu_{e}}$, $m_{\nu_{e}}<
0.8~{\rm eV}/c^{2}$. Here we explore the implications of combining the KATRIN
upper bound using a previously inferred lower bound on the smallest neutrino
mass state, $m_{i,{\rm min}}\gtrsim 0.4~{\rm eV}/c^{2}$ implied by the
stability of white dwarfs and neutron stars in the presence of long-range
many-body neutrino-exchange forces. By combining a revised lower bound estimate
with the expected final upper bound from KATRIN, we find that the available
parameter space for $m_{\nu_{e}}$ may be closed completely within the next few
years. We then extend the argument when a single light sterile neutrino flavor
is present to set a lower mass limit on sterile neutrinos.
Damping of neutrino oscillations, decoherence and the lengths of
neutrino wave packets
2208.03736 [abs] [pdf]
[abstract]
by Evgeny Akhmedov and Alexei Y. Smirnov.
Spatial separation of the wave packets (WPs) of neutrino mass eigenstates
leads to decoherence and damping of neutrino oscillations. Damping can also be
caused by finite energy resolution of neutrino detectors or, in the case of
experiments with radioactive neutrino sources, by finite width of the emitted
neutrino line. We study in detail these two types of damping effects using
reactor neutrino experiments and experiments with radioactive $^{51}$Cr source
as examples. We demonstrate that the effects of decoherence by WP separation
can always be incorporated into a modification of the energy resolution
function of the detector and so are intimately entangled with it. We estimate
for the first time the lengths $\sigma_x$ of WPs of reactor neutrinos and
neutrinos from a radioactive $^{51}$Cr source. The obtained values, $\sigma_x =
(2\times 10^{-5} - 1.4\times 10^{-4})$ cm, are at least six orders of magnitude
larger than the currently available experimental lower bounds. We conclude that
effects of decoherence by WP separation cannot be probed in reactor and
radioactive source experiments.
Impact of Nuclear effects in Energy Reconstruction Methods on
Sensitivity of Neutrino Oscillation Parameters at NO$ν$A experiment
2208.03681 [abs] [pdf]
[abstract]
by Paramita Deka, Jaydip Singh, and Kalpana Bora.
Long baseline (LBL) neutrino experiments aim to measure the neutrino
oscillation parameters to high precision. These experiments use nuclear targets
for neutrino scattering and hence are inflicted with complexities of nuclear
effects. Nuclear effects and their percolation into sensitivity measurement of
neutrino oscillations parameters are not yet fully understood and therefore
need to be dealt with carefully. In a recent work [1], we reported some results
on this for NO$\nu$A experiment using the kinematic method of neutrino energy
reconstruction, where it was observed that the nuclear effects are important in
sensitivity analysis, and inclusion of realistic detector setup specifications
increases uncertainty in this analysis as compared to ideal detector case. With
this motivation, in this work, we use two methods of neutrino energy
reconstruction - kinematic and calorimetric, including the nuclear effects, and
study their impact on sensitivity analysis. We consider nuclear interactions
such as RPA and 2p2h and compare two energy reconstruction methods with
reference to events generation, measurement of neutrino oscillation parameters
$\Delta m_{32}^2$ and $\theta_{23}$ for disappearance channel, mass hierarchy
sensitivity, and CP-violation sensitivity for appearance channel of the
NO$\nu$A experiment. It is observed that with an ideal detector setup, the
kinematic method shows significant dependence on nuclear effects compared to
the calorimetric method. We also investigate the impact of realistic detector
setup for NO$\nu$A in these two methods (with nuclear effects) and find that
the calorimetric method shows more bias (uncertainty increases) in sensitivity
contours, as compared to the kinematic method. This is found to be true for
both the mass hierarchies and for both neutrino and antineutrino incoming
beams.
Bounds on ultralight bosons from the Event Horizon Telescope observation
of Sgr A$^*$
2208.03530 [abs] [pdf]
[abstract]
by Akash Kumar Saha, [and 5 more]Priyank Parashari, Tarak Nath Maity, Abhishek Dubey, Subhadip Bouri, and Ranjan Laha [hide authors].
Recent observation of Sagittarius A$^*$ (Sgr A$^*$) by the Event Horizon
Telescope (EHT) collaboration has uncovered various unanswered questions in
black hole (BH) physics. Besides, it may also probe various beyond the Standard
Model (BSM) scenarios. One of the most profound possibilities is the search for
ultralight bosons (ULBs) using BH superradiance (SR). EHT observations imply
that Sgr A$^*$ has a non-zero spin. Using this observation, we derive bounds on
the mass of ULBs with purely gravitational interactions. Considering
self-interacting ultralight axions, we constrain new regions in the parameter
space of decay constant, for a certain spin of Sgr A$^*$. Future observations
of various spinning BHs can improve the present constraints on ULBs.
July 2022
Unveiling the outer core composition with neutrino oscillation
tomography
2208.00532 [abs] [pdf]
[abstract]
by L. Maderer, [and 4 more]E. Kaminski, J. A. B. Coelho, S. Bourret, and V. Van Elewyck [hide authors].
In the last 70 years, geophysics has established that the Earth's outer core
is an FeNi alloy containing a few percent of light elements, whose nature and
amount remain controversial today. Besides the classical combinations of
silicon and oxygen, hydrogen has been advocated as the only light element that
could account alone for both the density and velocity profiles of the outer
core. Here we show how this question can be addressed from an independant
viewpoint, by exploiting the tomographic information provided by atmospheric
neutrinos, weakly-interacting particles produced in the atmosphere and
constantly traversing the Earth. We evaluate the potential of the upcoming
generation of atmospheric neutrino detectors for such a measurement, showing
that they could efficiently detect the presence of 1 wt% of hydrogen in an FeNi
core in 50 years of concomitant data taking. We then identify the main
requirements for a next-generation detector to perform this measurement in a
few years timescale, with the further capability to efficiently discriminate
between FeNiH and FeNiSi(x)O(y) models in less than 15 years.
The brightest galaxies at Cosmic Dawn
2207.14808 [abs] [pdf]
[abstract]
by Charlotte A. Mason, Michele Trenti, and Tommaso Treu.
Recent JWST observations suggest an excess of $z\gtrsim10$ galaxy candidates
above most theoretical models. Here, we explore how the interplay between halo
formation timescales, star formation efficiency and dust attenuation affects
the properties and number densities of galaxies we can detect in the early
universe. We calculate the theoretical upper limit on the UV luminosity
function, assuming star formation is 100% efficient and all gas in halos is
converted into stars, and that galaxies are at the peak age for UV emission
(~10 Myr). This upper limit is ~4 orders of magnitude greater than current
observations, implying these are fully consistent with star formation in
$\Lambda$CDM cosmology. In a more realistic model, we use the distribution of
halo formation timescales derived from extended Press-Schechter theory as a
proxy for star formation rate (SFR). We predict that the galaxies observed so
far at $z\gtrsim10$ are dominated by those with the fastest formation
timescales, and thus most extreme SFRs and young ages. These galaxies can be
upscattered by ~1.5 mag compared to the median UV magnitude vs halo mass
relation. This likely introduces a selection effect at high redshift whereby
only the youngest ($\lesssim$10 Myr), most highly star forming galaxies
(specific SFR$\gtrsim$30 Gyr$^{-1}$) have been detected so far. Furthermore,
our modelling suggests that redshift evolution at the bright end of the UV
luminosity function is substantially affected by the build-up of dust
attenuation. We predict that deeper JWST observations (reaching m~30) will
reveal more typical galaxies with relatively older ages (~100 Myr) and less
extreme specific SFRs (~10 Gyr$^{-1}$ for a $M_\mathrm{UV}$ ~ -20 galaxy at
z~10).
Enhanced Small-Scale Structure in the Cosmic Dark Ages
2207.14735 [abs] [pdf]
[abstract]
by Derek Inman and Kazunori Kohri.
We consider the consequences of a matter power spectrum which rises on small
scales until eventually being cutoff by microphysical processes associated with
the particle nature of dark matter. Evolving the perturbations of a weakly
interacting massive particle from before decoupling until deep in the nonlinear
regime, we show that nonlinear structure can form abundantly at very high
redshifts. In such a scenario, dark matter annihilation is substantially
increased after matter-radiation equality. Furthermore, since the power
spectrum can be increased over a broad range of scales, the first star forming
halos may form earlier than usual as well. The next challenge is determining
how early Universe observations may constrain such enhanced dark matter
perturbations.
The Profiled Feldman-Cousins technique for confidence interval
construction in the presence of nuisance parameters
2207.14353 [abs] [pdf]
[abstract]
by M. A. Acero, [and 220 more]B. Acharya, P. Adamson, L. Aliaga, N. Anfimov, A. Antoshkin, E. Arrieta-Diaz, L. Asquith, A. Aurisano, A. Back, C. Backhouse, M. Baird, N. Balashov, P. Baldi, B. A. Bambah, S. Bashar, A. Bat, K. Bays, R. Bernstein, V. Bhatnagar, D. Bhattarai, B. Bhuyan, J. Bian, A. C. Booth, R. Bowles, B. Brahma, C. Bromberg, N. Buchanan, A. Butkevich, S. Calvez, T. J. Carroll, E. Catano-Mur, A. Chatla, R. Chirco, B. C. Choudhary, S. Choudhary, A. Christensen, T. E. Coan, M. Colo, L. Cremonesi, G. S. Davies, P. F. Derwent, P. Ding, Z. Djurcic, M. Dolce, D. Doyle, D. Dueñas Tonguino, E. C. Dukes, A. Dye, R. Ehrlich, M. Elkins, E. Ewart, G. J. Feldman, P. Filip, J. Franc, M. J. Frank, H. R. Gallagher, R. Gandrajula, F. Gao, A. Giri, R. A. Gomes, M. C. Goodman, V. Grichine, M. Groh, R. Group, B. Guo, A. Habig, F. Hakl, A. Hall, J. Hartnell, R. Hatcher, H. Hausner, M. He, K. Heller, V Hewes, A. Himmel, B. Jargowsky, J. Jarosz, F. Jediny, C. Johnson, M. Judah, I. Kakorin, D. M. Kaplan, A. Kalitkina, J. Kleykamp, O. Klimov, L. W. Koerner, L. Kolupaeva, S. Kotelnikov, R. Kralik, Ch. Kullenberg, M. Kubu, A. Kumar, C. D. Kuruppu, V. Kus, T. Lackey, K. Lang, P. Lasorak, J. Lesmeister, S. Lin, A. Lister, J. Liu, M. Lokajicek, J. M. C. Lopez, R. Mahji, S. Magill, M. Manrique Plata, W. A. Mann, M. T. Manoharan, M. L. Marshak, M. Martinez-Casales, V. Matveev, B. Mayes, B. Mehta, M. D. Messier, H. Meyer, T. Miao, V. Mikola, W. H. Miller, S. Mishra, S. R. Mishra, A. Mislivec, R. Mohanta, A. Moren, A. Morozova, W. Mu, L. Mualem, M. Muether, K. Mulder, D. Naples, A. Nath, N. Nayak, S. Nelleri, J. K. Nelson, R. Nichol, E. Niner, A. Norman, A. Norrick, T. Nosek, H. Oh, A. Olshevskiy, T. Olson, J. Ott, A. Pal, J. Paley, L. Panda, R. B. Patterson, G. Pawloski, D. Pershey, O. Petrova, R. Petti, D. D. Phan, R. K. Plunkett, A. Pobedimov, J. C. C. Porter, A. Rafique, L. R. Prais, V. Raj, M. Rajaoalisoa, B. Ramson, B. Rebel, P. Rojas, P. Roy, V. Ryabov, O. Samoylov, M. C. Sanchez, S. Sánchez Falero, P. Shanahan, P. Sharma, S. Shukla, A. Sheshukov, I. Singh, P. Singh, V. Singh, E. Smith, J. Smolik, P. Snopok, N. Solomey, A. Sousa, K. Soustruznik, M. Strait, L. Suter, A. Sutton, S. Swain, C. Sweeney, A. Sztuc, B. Tapia Oregui, P. Tas, B. N. Temizel, T. Thakore, R. B. Thayyullathil, J. Thomas, E. Tiras, J. Tripathi, J. Trokan-Tenorio, Y. Torun, J. Urheim, P. Vahle, Z. Vallari, J. Vasel, T. Vrba, M. Wallbank, T. K. Warburton, M. Wetstein, D. Whittington, D. A. Wickremasinghe, T. Wieber, J. Wolcott, M. Wrobel, W. Wu, Y. Xiao, B. Yaeggy, A. Yallappa Dombara, A. Yankelevich, K. Yonehara, S. Yu, Y. Yu, S. Zadorozhnyy, J. Zalesak, Y. Zhang, and R. Zwaska [hide authors].
Measuring observables to constrain models using maximum-likelihood estimation
is fundamental to many physics experiments. The Profiled Feldman-Cousins method
described here is a potential solution to common challenges faced in
constructing accurate confidence intervals: small datasets, bounded parameters,
and the need to properly handle nuisance parameters. This method achieves more
accurate frequentist coverage than other methods in use, and is generally
applicable to the problem of parameter estimation in neutrino oscillations and
similar measurements. We describe an implementation of this method in the
context of the NOvA experiment.
Unravelling the formation of the first supermassive black holes with the
SKA pulsar timing array
2207.14309 [abs] [pdf]
[abstract]
by Hamsa Padmanabhan and Abraham Loeb.
Galaxy mergers at high redshifts trigger the activity of their central
supermassive black holes, eventually also leading to their coalescence -- and a
potential source of low-frequency gravitational waves detectable by the SKA
Pulsar Timing Array (PTA). Two key parameters related to the fuelling of black
holes are the Eddington ratio of quasar accretion $\eta_{\rm Edd}$, and the
radiative efficiency of the accretion process, $\epsilon$ (which affects the
so-called active lifetime of the quasar, $t_{\rm QSO}$). We forecast the regime
of detectability of gravitational wave events with SKA PTA, finding the
associated binaries to have orbital periods on the order of weeks to years,
observable through relativistic Doppler velocity boosting and/or optical
variability of their light curves. Combining the SKA regime of detectability
with the latest observational constraints on high-redshift black hole mass and
luminosity functions, and theoretically motivated prescriptions for the merger
rates of dark matter haloes, we forecast the number of active counterparts of
SKA PTA events expected as a function of primary black hole mass at $z \gtrsim
6$. We find that the quasar counterpart of the most massive black holes will be
${uniquely \ localizable}$ within the SKA PTA error ellipse at $z \gtrsim 6$.
We also forecast the number of expected counterparts as a function of the
quasars' Eddington ratio and active lifetime. Our results show that SKA PTA
detections can place robust constraints on the seeding and growth mechanisms of
the first supermassive black holes.
Jupiter missions as probes of dark matter
2207.13709 [abs] [pdf]
[abstract]
by Lingfeng Li and JiJi Fan.
Jupiter, the fascinating largest planet in the solar system, has been visited
by nine spacecraft, which have collected a significant amount of data about
Jovian properties. In this paper, we show that one type of the in situ
measurements on the relativistic electron fluxes could be used to probe dark
matter (DM) and dark mediator between the dark sector and our visible world.
Jupiter, with its immense weight and cool core, could be an ideal capturer for
DM with masses around the GeV scale. The captured DM particles could annihilate
into long-lived dark mediators such as dark photons, which subsequently decay
into electrons and positrons outside Jupiter. The charged particles, trapped by
the Jovian magnetic field, have been measured in Jupiter missions such as the
Galileo probe and the Juno orbiter. We use the data available to set upper
bounds on the cross section of DM scattering off nucleons, $\sigma_{\chi n}$,
for dark mediators with lifetime of order ${\cal O}(0.1-1)$s. The results show
that data from Jupiter missions already probe regions in the parameter space
un- or under-explored by existing DM searches, e.g., constrain $\sigma_{\chi
n}$ of order $(10^{-40} - 10^{-38})$ cm$^2$ for 1 GeV DM dominantly
annihilating into $e^+e^-$ through dark mediators. This study serves as an
example and an initial step to explore the full physics potential of the large
planetary datasets from Jupiter missions. We also outline several other
potential directions related to secondary products of electrons, positron
signals and solar axions.
Limits on the cosmic neutrino background
2207.12413 [abs] [pdf]
[abstract]
by Martin Bauer and Jack D. Shergold.
We present the first comprehensive discussion of constraints on the cosmic
neutrino background (C$\nu$B) overdensity, including theoretical, experimental
and cosmological limits for a wide range of neutrino masses and temperatures.
Additionally, we calculate the sensitivities of future direct and indirect
relic neutrino detection experiments and compare the results with the existing
constraints, extending several previous analyses by taking into account that
the C$\nu$B reference frame may not be aligned with that of the Earth. The
Pauli exclusion principle strongly disfavours overdensities $\eta_\nu \gg 1$ at
small neutrino masses, but allows for overdensities $\eta_{\nu}\lesssim 125$ at
the KATRIN mass bound $m_{\nu} \simeq 0.8\,\mathrm{eV}$. On the other hand,
cosmology strongly favours $0.2 \lesssim \eta_{\nu} \lesssim 3.5$ in all
scenarios. We find that direct detection proposals are capable of observing the
C$\nu$B without a significant overdensity for neutrino masses $m_{\nu} \gtrsim
50\,\mathrm{meV}$, but require an overdensity $\eta_{\nu} \gtrsim 3\times 10^5$
outside of this range. We also demonstrate that relic neutrino detection
proposals are sensitive to the helicity composition of the C$\nu$B, whilst some
may be able to distinguish between Dirac and Majorana neutrinos.
Dark Matter Constraints from the Eccentric Supermassive Black Hole
Binary OJ 287
2207.10021 [abs] [pdf]
[abstract]
by Ahmad Alachkar, John Ellis, and Malcolm Fairbairn.
OJ 287 is a blazar thought to be a binary system containing a ~ 18 billion
solar mass primary black hole accompanied by a ~ 150 million solar mass
secondary black hole in an eccentric orbit, which triggers electromagnetic
flares twice in every ~ 12 year orbital period when it traverses the accretion
disk of the primary. The times of these emissions are consistent with the
predictions of general relativity calculated to the 4.5th post-Newtonian order.
The orbit of the secondary black hole samples the gravitational field at
distances between O(10) and O(50) Schwarzschild radii around the primary, and
hence is sensitive to the possible presence of a dark matter spike around it.
We find that the agreement of general-relativistic calculations with the
measured timings of flares from OJ 287 constrains the mass of such a spike to <
3% of the primary mass.
Do Pulsar and Fast Radio Burst dispersion measures obey Benford's law?
2207.09696 [abs] [pdf]
[abstract]
by Pragna Mamidipaka and Shantanu Desai.
We check if the first significant digit of the dispersion measure of pulsars
and Fast Radio Bursts (using the CHIME catalog) is consistent with the Benford
distribution. We find a large disagreement with Benford's law with $\chi^2$
close to 80 for 8 degrees of freedom for both these aforementioned datasets.
This corresponds to a discrepancy of about 7$\sigma$. Therefore, we conclude
that the dispersion measures of pulsars and FRBs do not obey Benford's law.
Diffuse supernova neutrino background
2207.09632 [abs] [pdf]
[abstract]
by Anna M. Suliga.
Neutrinos are the second most ubiquitous Standard Model particles in the
universe. On the other hand, they are also the ones least likely to interact.
Connecting these two points suggests that when a neutrino is detected, it can
divulge unique pieces of information about its source. Among the known neutrino
sources, core-collapse supernovae in the universe are the most abundant for
MeV-energies. On average, a single collapse happens every second in the
observable universe and produces $10^{58}$ neutrinos. The flux of neutrinos
reaching the Earth from all the core-collapse supernovae in the universe is
known as diffuse supernova neutrino background. In this Chapter, the basic
prediction for the diffuse supernova neutrino background is presented. This
includes a discussion of an average neutrino signal from a core-collapse
supernova, variability of that signal due to the remnant formed in the process,
and uncertainties connected to the other astrophysical parameters determining
the diffuse flux, such as cosmological supernova rate. In addition, the current
experimental limits and detection perspectives of diffuse supernova neutrino
background are reported.
Massive neutrino self-interactions and inflation
2207.07142 [abs] [pdf]
[abstract]
by Shouvik Roy Choudhury, Steen Hannestad, and Thomas Tram.
Certain inflationary models like Natural inflation (NI) and Coleman-Weinberg
inflation (CWI) are disfavoured by cosmological data in the standard
$\Lambda\textrm{CDM}+r$ model (where $r$ is the scalar-to-tensor ratio), as
these inflationary models predict the regions in the $n_s-r$ parameter space
that are excluded by the cosmological data at more than 2$\sigma$ (here $n_s$
is the scalar spectral index). The same is true for single field inflationary
models with an inflection point that can account for all or majority of dark
matter in the form of PBHs (primordial black holes). Cosmological models
incorporating strongly self-interacting neutrinos (with a heavy mediator) are,
however, known to prefer lower $n_s$ values compared to the $\Lambda\rm CDM$
model. Considering such neutrino self-interactions can, thus, open up the
parameter space to accommodate the above inflationary models. In this work, we
implement the massive neutrino self-interactions with a heavy mediator in two
different ways: flavour-universal (among all three neutrinos), and
flavour-specific (involving only one neutrino species). We implement the new
interaction in both scalar and tensor perturbation equations of neutrinos.
Interestingly, we find that the current cosmological data can support the
aforementioned inflationary models at 2$\sigma$ in the presence of such
neutrino self-interactions.
Model marginalized constraints on neutrino properties from cosmology
2207.05167 [abs] [pdf]
[abstract]
by Eleonora di Valentino, Stefano Gariazzo, and Olga Mena.
We present robust, model-marginalized limits on both the total neutrino mass
($\sum m_\nu$) and abundance ($N_{\rm eff}$) to minimize the role of
parameterizations, priors and models when extracting neutrino properties from
cosmology. The cosmological observations we consider are CMB temperature
fluctuation and polarization measurements, Supernovae Ia luminosity distances,
BAO observations and determinations of the growth rate parameter from the Data
Release 16 of the Sloan Digital Sky Survey IV. The degenerate neutrino mass
spectrum (which implies $\sum m_\nu>0$) is weakly (moderately) preferred over
the normal and inverted hierarchy possibilities, which imply the priors $\sum
m_\nu>0.06$ and $\sum m_\nu>0.1$ eV respectively. Concerning the underlying
cosmological model, the $\Lambda$CDM minimal scenario is almost always strongly
preferred over the possible extensions explored here. The most constraining
$95\%$ CL bound on the total neutrino mass in the $\Lambda$CDM+$\sum m_\nu$
picture is $\sum m_\nu< 0.087$ eV. The parameter $N_{\rm eff}$ is restricted to
$3.08\pm 0.17$ ($68\%$ CL) in the $\Lambda$CDM+$N_{\rm eff}$ model. These
limits barely change when considering the $\Lambda$CDM+$\sum m_\nu$+$N_{\rm
eff}$ scenario. Given the robustness and the strong constraining power of the
cosmological measurements employed here, the model-marginalized posteriors
obtained considering a large spectra of non-minimal cosmologies are very close
to the previous bounds, obtained within the $\Lambda$CDM framework in the
degenerate neutrino mass spectrum. Future cosmological measurements may improve
the current Bayesian evidence favouring the degenerate neutrino mass spectra,
challenging therefore the consistency between cosmological neutrino mass bounds
and oscillation neutrino measurements, and potentially suggesting a more
complicated cosmological model and/or neutrino sector.
Chern-Simons Gravity and Neutrino Self-Interactions
2207.05094 [abs] [pdf]
[abstract]
by Stephon Alexander and Cyril Creque-Sarbinowski.
Dynamical Chern-Simons gravity (dCS) is a four-dimensional parity-violating
extension of general relativity. Current models predict the effect of this
extension to be negligible due to large decay constants $f$ close to the scale
of grand unified theories. Here, we present a construction of dCS allowing for
much smaller decay constants, ranging from sub-eV to Planck scales.
Specifically, we show that if there exists a fermion species with strong
self-interactions, the short-wavelength fermion modes form a bound state. This
bound state can then undergo dynamical symmetry breaking and the resulting
pseudoscalar develops Yukawa interactions with the remaining long-wavelength
fermion modes. Due to this new interaction, loop corrections with gravitons
then realize a linear coupling between the pseudoscalar and the gravitational
Chern-Simons term. The strength of this coupling is set by the Yukawa coupling
constant divided by the fermion mass. Therefore, since self-interacting
fermions with small masses are ideal, we identify neutrinos as promising
candidates. For example, if a neutrino has a mass $m_\nu \lesssim {\rm meV}$
and the Yukawa coupling is order unity, the dCS decay constant can be as small
as $f \sim 10^3 m_\nu \lesssim {\rm eV}$. We discuss other potential choices
for fermions.
Search for Astrophysical Neutrinos from 1FLE Blazars with IceCube
2207.04946 [abs] [pdf]
[abstract]
by R. Abbasi, [and 382 more]M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, J. M. Alameddine, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, V. Basu, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. Benda, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Y. Book, J. Borowka, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, F. Bradascio, J. Braun, B. Brinson, S. Bron, J. Brostean-Kaiser, R. T. Burley, R. S. Busse, M. A. Campana, E. G. Carnie-Bronca, C. Chen, Z. Chen, D. Chirkin, K. Choi, B. A. Clark, L. Classen, A. Coleman, G. H. Collin, A. Connolly, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, C. Dappen, P. Dave, C. De Clercq, J. J. DeLaunay, D. Delgado López, H. Dembinski, K. Deoskar, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, H. Dujmovic, M. A. DuVernois, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, K. L. Fan, A. R. Fazely, A. Fedynitch, N. Feigl, S. Fiedlschuster, A. T. Fienberg, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, A. Garcia, S. Garrappa, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glauch, T. Glüsenkamp, N. Goehlke, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, S. Griswold, C. Günther, P. Gutjahr, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, H. Hamdaoui, M. Ha Minh, K. Hanson, J. Hardin, A. A. Harnisch, P. Hatch, A. Haungs, K. Helbing, J. Hellrung, F. Henningsen, E. C. Hettinger, L. Heuermann, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, K. Hoshina, W. Hou, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, K. Hymon, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, M. Jin, B. J. P. Jones, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, L. Kardum, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, J. L. Kelley, A. Kheirandish, K. Kin, J. Kiryluk, S. R. Klein, A. Kochocki, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, T. Kozynets, E. Krupczak, E. Kun, N. Kurahashi, N. Lad, C. Lagunas Gualda, M. J. Larson, F. Lauber, J. P. Lazar, J. W. Lee, K. Leonard, A. Leszczyńska, M. Lincetto, Q. R. Liu, M. Liubarska, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, S. Mancina, W. Marie Sainte, I. C. Mariş, I. Martinez-Soler, R. Maruyama, S. McCarthy, T. McElroy, F. McNally, J. V. Mead, K. Meagher, S. Mechbal, A. Medina, M. Meier, S. Meighen-Berger, Y. Merckx, J. Micallef, D. Mockler, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, T. Mukherjee, R. Naab, R. Nagai, U. Naumann, J. Necker, L. V. Nguyen, H. Niederhausen, M. U. Nisa, S. C. Nowicki, A. Obertacke Pollmann, M. Oehler, B. Oeyen, A. Olivas, J. Osborn, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, L. Paul, C. Pérez de los Heros, L. Peters, J. Peterson, S. Philippen, S. Pieper, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, B. Pries, G. T. Przybylski, C. Raab, J. Rack-Helleis, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, Z. Rechav, A. Rehman, P. Reichherzer, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, E. J. Roberts, S. Robertson, S. Rodan, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, J. Saffer, D. Salazar-Gallegos, P. Sampathkumar, S. E. Sanchez Herrera, A. Sandrock, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Schaufel, H. Schieler, S. Schindler, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, G. Schwefer, S. Sclafani, D. Seckel, S. Seunarine, A. Sharma, S. Shefali, N. Shimizu, M. Silva, B. Skrzypek, B. Smithers, R. Snihur, J. Soedingrekso, A. Sogaard, D. Soldin, C. Spannfellner, G. M. Spiczak, C. Spiering, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, T. Stezelberger, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, S. Ter-Antonyan, W. G. Thompson, J. Thwaites, S. Tilav, K. Tollefson, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, J. P. Twagirayezu, B. Ty, M. A. Unland Elorrieta, M. Unland Elorrieta, K. Upshaw, N. Valtonen-Mattila, J. Vandenbroucke, N. van Eijndhoven, D. Vannerom, J. van Santen, J. Veitch-Michaelis, S. Verpoest, C. Walck, W. Wang, T. B. Watson, C. Weaver, P. Weigel, A. Weindl, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. H. Wiebusch, N. Willey, D. R. Williams, M. Wolf, G. Wrede, J. Wulff, X. W. Xu, J. P. Yanez, E. Yildizci, S. Yoshida, S. Yu, T. Yuan, Z. Zhang, and P. Zhelnin [hide authors].
The majority of astrophysical neutrinos have undetermined origins. The
IceCube Neutrino Observatory has observed astrophysical neutrinos but has not
yet identified their sources. Blazars are promising source candidates, but
previous searches for neutrino emission from populations of blazars detected in
$\gtrsim$ GeV gamma-rays have not observed any significant neutrino excess.
Recent findings in multi-messenger astronomy indicate that high-energy photons,
co-produced with high-energy neutrinos, are likely to be absorbed and reemitted
at lower energies. Thus, lower-energy photons may be better indicators of
TeV-PeV neutrino production. This paper presents the first time-integrated
stacking search for astrophysical neutrino emission from MeV-detected blazars
in the first Fermi-LAT low energy catalog (1FLE) using ten years of IceCube
muon-neutrino data. The results of this analysis are found to be consistent
with a background-only hypothesis. Assuming an E$^{-2}$ neutrino spectrum and
proportionality between the blazars' MeV gamma-ray fluxes and TeV-PeV neutrino
flux, the upper limit on the 1FLE blazar energy-scaled neutrino flux is
determined to be $1.64 \times 10^{-12}$ TeV cm$^{-2}$ s$^{-1}$ at 90%
confidence level. This upper limit is approximately 1% of IceCube's diffuse
muon-neutrino flux measurement.
A First Search for Solar $^8$B Neutrino in the PandaX-4T Experiment
using Neutrino-Nucleus Coherent Scattering
2207.04883 [abs] [pdf]
[abstract]
by Wenbo Ma, [and 90 more]Abdusalam Abdukerim, Chen Cheng, Zihao Bo, Wei Chen, Xun Chen, Yunhua Chen, Zhaokan Cheng, Xiangyi Cui, Yingjie Fan, Deqing Fang, Changbo Fu, Mengting Fu, Lisheng Geng, Karl Giboni, Linhui Gu, Xuyuan Guo, Chencheng Han, Ke Han, Changda He, Jinrong He, Di Huang, Yanlin Huang, Zhou Huang, Ruquan Hou, Xiangdong Ji, Yonglin Ju, Chenxiang Li, Jiafu Li, Mingchuan Li, Shu Li, Shuaijie Li, Qing Lin, Jianglai Liu, Xiaoying Lu, Lingyin Luo, Yunyang Luo, Yugang Ma, Yajun Mao, Nasir Shaheed, Yue Meng, Xuyang Ning, Ningchun Qi, Zhicheng Qian, Xiangxiang Ren, Changsong Shang, Xiaofeng Shang, Guofang Shen, Lin Si, Wenliang Sun, Andi Tan, Yi Tao, Anqing Wang, Meng Wang, Qiuhong Wang, Shaobo Wang, Siguang Wang, Wei Wang, Xiuli Wang, Zhou Wang, Yuehuan Wei, Mengmeng Wu, Weihao Wu, Jingkai Xia, Mengjiao Xiao, Xiang Xiao, Pengwei Xie, Binbin Yan, Xiyu Yan, Jijun Yang, Yong Yang, Chunxu Yu, Jumin Yuan, Ying Yuan, Zhe Yuan, Xinning Zeng, Dan Zhang, Minzhen Zhang, Peng Zhang, Shibo Zhang, Shu Zhang, Tao Zhang, Yingxin Zhang, Yuanyuan Zhang, Li Zhao, Qibin Zheng, Jifang Zhou, Ning Zhou, Xiaopeng Zhou, Yong Zhou, and Yubo Zhou [hide authors].
A search for interactions from solar $^8$B neutrinos elastically scattering
off xenon nuclei using PandaX-4T commissioning data is reported. The energy
threshold of this search is further lowered compared with the previous search
for dark matter, with various techniques utilized to suppress the background
that emerges from data with the lowered threshold. A blind analysis is
performed on the data with an effective exposure of 0.48 tonne$\cdot$year, and
no significant excess of events is observed. Among results obtained using the
neutrino-nucleus coherent scattering, our results give the best constraint on
the solar $^8$B neutrino flux. We further provide a more stringent limit on the
cross section between dark matter and nucleon in the mass range from 3 to 9
GeV/c$^2$.
Neutrino Mass Ordering -- Circumventing the Challenges using Synergy
between T2HK and JUNO
2207.04784 [abs] [pdf]
[abstract]
by Sandhya Choubey, Monojit Ghosh, and Deepak Raikwal.
One of the major open problems of neutrino physics is MO (mass ordering). We
discuss the prospects of measuring MO with two under-construction experiments
T2HK and JUNO. JUNO alone is expected to measure MO with greater than $3\sigma$
significance as long as certain experimental challenges are met. In particular,
JUNO needs better than 3$\%$ energy resolution for MO measurement. On the other
hand, T2HK has rather poor prospects at measuring the MO, especially for
certain ranges of the CP violating parameter $\delta_{\rm CP}$, posing a major
drawback for T2HK. In this letter we show that the synergy between JUNO and
T2HK will bring two-fold advantage. Firstly, the synergy between the two
experiments helps us determine the MO at a very high significance. With the
baseline set-up of the two experiments, we have a greater than $9\sigma$
determination of the MO for all values of $\delta_{\rm CP}$. Secondly, the
synergy also allows us to relax the constraints on the two experiments. We show
that JUNO, could perform extremely well even for energy resolution of 5$\%$,
while for T2HK the MO problem with "bad" values of $\delta_{\rm CP}$ goes away.
The MO sensitivity for the combined analysis is expected to be greater than
$6\sigma$ for all values of $\delta_{\rm CP}$ and with just 5$\%$ energy
resolution for JUNO.
Solar $\barν_e$ flux: Revisiting bounds on neutrino magnetic moments
and solar magnetic field
2207.04516 [abs] [pdf]
[abstract]
by Evgeny Akhmedov and Pablo Martínez-Miravé.
The interaction of neutrino transition magnetic dipole moments with magnetic
fields can give rise to the phenomenon of neutrino spin-flavour precession
(SFP). For Majorana neutrinos, the combined action of SFP of solar neutrinos
and flavour oscillations would manifest itself as a small, yet potentially
detectable, flux of electron antineutrinos coming from the Sun. Non-observation
of such a flux constrains the product of the neutrino magnetic moment $\mu$ and
the strength of the solar magnetic field $B$. We derive a simple analytical
expression for the expected $\bar{\nu}_e$ appearance probability in the
three-flavour framework and we use it to revisit the existing experimental
bounds on $\mu B$. A full numerical calculation has also been performed to
check the validity of the analytical result. We also present our numerical
results in energy-binned form, convenient for analyses of the data of the
current and future experiments searching for the solar $\bar{\nu}_e$ flux. In
addition, we give a comprehensive compilation of other existing limits on
neutrino magnetic moments and of the expressions for the probed effective
magnetic moments in terms of the fundamental neutrino magnetic moments and
leptonic mixing parameters.
Predicting leptonic CP violation via minimization of neutrino
entanglement
2207.03303 [abs] [pdf]
[abstract]
by Gonçalo M. Quinta, Alexandre Sousa, and Yasser Omar.
We show how a minimization principle of quantum entanglement between the
oscillating flavors of a neutrino leads to a unique prediction for the
CP-violation phase in the neutrino sector without assuming extra symmetries in
the Standard Model. We find a theoretical prediction consistent with either no
CP-violation or a very small presence of it.
Study of matter effects in the presence of sterile neutrino using OMSD
approximation
2207.03249 [abs] [pdf]
[abstract]
by Kiran Sharma and Sudhanwa Patra.
We discuss the transition and survival probabilities in $3+1$ neutrino flavor
mixing scenario in presence of matter effects. We adopt the well-known OMSD(One
Mass Scale Dominance) approximation to carry out our analysis. After that we
perform series expansion about $\sin \theta_{13}$ term upto second order. We
find that our results are consistent with the already existing $\alpha - \sin
\theta_{13}$ approximated relations in the limit of vanishing $\alpha$ and
phases involving sterile neutrinos. We also figure out that survival transition
probability becomes independent of the fundamental and sterile CP phases under
our formalism. Hence, it provides us a new way to look at only matter effects
contribution to oscillation probability. Also, the transition probability at
the same time gives an independent study of CP-violation arising from the
sterile phases, in the vicinity of fundamental CP violation phase. We provide
the relation for the atmospheric probability in the presence of matter by
performing the series expansion upto linear order about parameter $A (= 2EV)$,
with V being the effective matter potential under OMSD approximation.
Imprints of flavor anomalies on neutrino oscillations through dark
matter halo
2207.02962 [abs] [pdf]
[abstract]
by Ashutosh Kumar Alok, Neetu Raj Singh Chundawat, and Arindam Mandal.
In this work we study the impact of new physics, stimulated by flavor
anomalies, on neutrino oscillations through dense dark matter halo. Inspired by
a model where a Majorana dark matter fermion and two new scalar fields
contribute to $b \to s \mu^+ \mu^-$ transition at the one loop level, we study
the impact of neutrino-dark matter interaction on the oscillation patterns of
ultra-high energy cosmic neutrinos passing through this muonphilic halo located
near the center of Milky Way. We find that due to this interaction, the flavor
ratios of neutrinos reaching earth would be different from that of vacuum
oscillations. We also consider a $Z'$ model driven by $L_{\mu}-L_{\tau}$
symmetry and containing a vector-like fermion as a dark matter candidate. It
was previously shown that for such a model, the three flavors of neutrinos
decouple from each other. This will render a flavor ratio similar to that of
vacuum oscillations. Therefore, the interaction of neutrinos with dense dark
matter halo can serve as an important tool to discriminate between flavor
models with a dark connection.
A New Probe of Relic Neutrino Clustering using Cosmogenic Neutrinos
2207.02860 [abs] [pdf]
[abstract]
by Vedran Brdar, [and 3 more]P. S. Bhupal Dev, Ryan Plestid, and Amarjit Soni [hide authors].
We propose a new probe of cosmic relic neutrinos (C$\nu$B) using their
resonant scattering against cosmogenic neutrinos. Depending on the lightest
neutrino mass and the energy spectrum of the cosmogenic neutrino flux, a
Standard Model vector meson (such as a hadronic $\rho$) resonance can be
produced via $\nu\bar{\nu}$ annihilation. This leads to a distinct absorption
feature in the cosmogenic neutrino flux at an energy solely determined by the
meson mass and the neutrino mass, apart from redshift. By numerical
coincidence, the position of the $\rho$-resonance overlaps with the originally
predicted peak of the Greisen-Zatsepin-Kuzmin (GZK) neutrino flux, which offers
an enhanced absorption effect at higher redshifts. We show that this absorption
feature in the GZK neutrino flux may be observable in future radio-based
neutrino observatories, such as IceCube-Gen2 radio, provided there exists a
large overdensity in the C$\nu$B distribution. This therefore provides a new
probe of C$\nu$B clustering at large redshifts, complementary to the laboratory
probes (such as KATRIN) at zero redshift.
Large Extra Dimensions and neutrino experiments
2207.02790 [abs] [pdf]
[abstract]
by D. V. Forero, [and 3 more]C. Giunti, C. A. Ternes, and O. Tyagi [hide authors].
The existence of Large Extra Dimensions can be probed in various neutrino
experiments. We analyze several neutrino data sets in a model with a dominant
large extra dimension. We show that the Gallium anomaly can be explained with
neutrino oscillations induced by the large extra dimension, but the region of
parameter space which is preferred by the Gallium anomaly is in tension with
the bounds from reactor rate data, as well as the data of Daya Bay and MINOS.
We also present bounds obtained from the analysis of the KATRIN data. We show,
that current experiments can put strong bounds on the size $R_{\text{ED}}$ of
the extra dimension: $R_{\text{ED}} < 0.20~\mu\text{m}$ and $R_{\text{ED}} <
0.10~\mu\text{m}$ at 90\% C.L. for normal and inverted ordering of the standard
neutrino masses, respectively.
Baseline and other effects for a sterile neutrino at DUNE
2207.02331 [abs] [pdf]
[abstract]
by J. T. Penedo and João Pulido.
We analyse the sensitivity of the Deep Underground Neutrino Experiment (DUNE)
to a sterile neutrino, combining information from both near and far detectors.
We quantify often-neglected effects which may impact the event rate estimation
in a 3+1 oscillation scenario. In particular, we find that taking into account
the information on the neutrino production point, in contrast to assuming a
point-like neutrino source, affects DUNE's sterile exclusion reach. Visible
differences remain after the inclusion of energy bin-to-bin uncorrelated
systematics. Instead, implementing exact oscillation formulae for near detector
events, including a two slab density profile, does not result in any visible
change in the sensitivity.
Double and multiple bangs at tau neutrino telescopes: A novel probe of
sphalerons with cosmogenic neutrinos
2207.02222 [abs] [pdf]
[abstract]
by Guo-yuan Huang.
In light of the exciting campaign of cosmogenic neutrino detection, we
investigate the double and multiple tau bangs detectable at future tau neutrino
telescopes. Such events are expected from the Standard Model (SM) higher-order
processes, which can be easily identified with broad techniques anticipated at
future tau neutrino telescopes. We find that SM perturbative processes can
already contribute observable double-bang events to telescopes with a
sensitivity of collecting $\mathcal{O}(100)$ cosmogenic neutrino events. The
detectable but suppressed rate in fact makes the double and multiple bangs an
excellent probe of SM unknowns and possible new physics beyond. As a case
study, the nonperturbative sphaleron process, which can copiously produce
multiple tau bangs, is explored.
Updated neutrino mass constraints from galaxy clustering and CMB
lensing-galaxy cross-correlation measurements
2207.01913 [abs] [pdf]
[abstract]
by Isabelle Tanseri, [and 4 more]Steffen Hagstotz, Sunny Vagnozzi, Elena Giusarma, and Katherine Freese [hide authors].
We revisit cosmological constraints on the sum of the neutrino masses $\Sigma
m_\nu$ from a combination of full-shape BOSS galaxy clustering [$P(k)$] data
and measurements of the cross-correlation between Planck Cosmic Microwave
Background (CMB) lensing convergence and BOSS galaxy overdensity maps
[$C^{\kappa \text{g}}_{\ell}$], using a simple but theoretically motivated
model for the scale-dependent galaxy bias in auto- and cross-correlation
measurements. We improve upon earlier related work in several respects,
particularly through a more accurate treatment of the correlation and
covariance between $P(k)$ and $C^{\kappa \text{g}}_{\ell}$ measurements. When
combining these measurements with Planck CMB data, we find a 95% confidence
level upper limit of $\Sigma m_\nu<0.14\,{\rm eV}$, while slightly weaker
limits are obtained when including small-scale ACTPol CMB data, in agreement
with our expectations. We confirm earlier findings that (once combined with CMB
data) the full-shape information content is comparable to the geometrical
information content in the reconstructed BAO peaks given the precision of
current galaxy clustering data, discuss the physical significance of our
inferred bias and shot noise parameters, and perform a number of robustness
tests on our underlying model. While the inclusion of $C^{\kappa
\text{g}}_{\ell}$ measurements does not currently appear to lead to substantial
improvements in the resulting $\Sigma m_{\nu}$ constraints, we expect the
converse to be true for near-future galaxy clustering measurements, whose shape
information content will eventually supersede the geometrical one.
June 2022
Dark photon superradiance quenched by dark matter
2206.12367 [abs] [pdf]
[abstract]
by Enrico Cannizzaro, [and 3 more]Laura Sberna, Andrea Caputo, and Paolo Pani [hide authors].
Black-hole superradiance has been used to place very strong bounds on a
variety of models of ultralight bosons such as axions, new light scalars, and
dark photons. It is common lore to believe that superradiance bounds are
broadly model independent and therefore pretty robust. In this work we show
however that superradiance bounds on dark photons can be challenged by simple,
compelling extensions of the minimal model. In particular, if the dark photon
populates a larger dark sector and couples to dark fermions playing the role of
dark matter, then superradiance bounds can easily be circumvented, depending on
the mass and (dark) charge of the dark matter.
Extracting the best physics sensitivity from T2HKK: A study on optimal
detector volume
2206.10320 [abs] [pdf]
[abstract]
by Papia Panda, [and 3 more]Monojit Ghosh, Priya Mishra, and Rukmani Mohanta [hide authors].
T2HK is an upcoming long-baseline experiment in Japan which will have two
water Cherenkov detector tanks of 187 kt volume each at distance of 295 km from
the source. An alternative project, T2HKK is also under consideration where one
of the water tanks will be moved to Korea at a distance of 1100 km. The flux at
295 km will cover the first oscillation maximum and the flux at 1100 km will
mainly cover the second oscillation maximum. As physics sensitivity at the dual
baseline rely on variation in statistics, dependence of systematic uncertainty,
effect of second oscillation maximum and matter density, 187 kt detector volume
at 295 km and 187 kt detector volume at 1100 km may not be the optimal
configuration of T2HKK. Therefore, we have tried to optimize the ratio of the
detector volume at both the locations by studying the interplay between the
above mentioned parameters. For the analysis of neutrino mass hierarchy, octant
of $\theta_{23}$ and CP precision, we have considered two values of
$\delta_{\rm{CP}}$ as 270$^\circ$ and $0^\circ$ and for CP violation we have
considered the value of $\delta_{\rm CP}= 270^\circ$. These values are
motivated by the current best-fit values of this parameter as obtained from the
experiments T2K and NO$\nu$A. Interestingly we find that if the systematic
uncertainty is negligible then the T2HK setup i.e., when both the detector
tanks are placed at 295 km gives the best results in terms of hierarchy
sensitivity at $\delta_{\rm CP}= 270^\circ$, octant sensitivity, CP violation
sensitivity and CP precision sensitivity at $\delta_{\rm CP}= 0^\circ$. For
current values of systematic errors, we find that neither T2HK, nor T2HKK setup
is giving better results for hierarchy, CP violation and CP precision
sensitivity. The optimal detector volume which is of the range between 255 kt
to 345 kt at 1100 km gives better results in those above mentioned parameters.
Probing non-standard neutrino interactions with a light boson from next
galactic and diffuse supernova neutrinos
2206.06852 [abs] [pdf]
[abstract]
by Kensuke Akita, Sang Hui Im, and Mehedi Masud.
Non-standard neutrino interactions with a massive boson can produce the
bosons in the core of core-collapse supernovae (SNe). After the emission of the
bosons from the SN core, their subsequent decays into neutrinos can modify the
SN neutrino flux. We show future observations of neutrinos from a next galactic
SN in Super-Kamiokande (SK) and Hyper-Kamiokande (HK) can probe
flavor-universal non-standard neutrino couplings to a light boson, improving
the previous limit from the SN 1987A neutrino burst by several orders of
magnitude. We also discuss sensitivity of the flavor-universal non-standard
neutrino interactions in future observations of diffuse neutrinos from all the
past SNe, known as the diffuse supernova neutrino background (DSNB). According
to our analysis, observations of the DSNB in HK, JUNO and DUNE experiments can
probe such couplings by a factor of $\sim 2$ beyond the SN 1987A constraint.
However, our result is also subject to a large uncertainty concerning the
precise estimation of the DSNB.
Symmetry in neutrino oscillation in matter with non-unitarity
2206.06474 [abs] [pdf]
[abstract]
by Hisakazu Minakata.
Recently we have developed a method called Symmetry Finder (SF) for hunting
the reparametrization symmetry in the three-neutrino system in matter. Here we
apply SF to the Denton {\it et al.} (DMP) perturbation theory extended by
including unitarity violation (UV), a possible low-energy manifestation of
physics beyond the $\nu$SM. Implementation of UV into the SF framework yields
the additional two very different constraints, which nonetheless allow
remarkably consistent solutions, the eight DMP-UV symmetries. Treatment of one
of the constraints, the genuine non-unitary part, leads to the key identity
which entails the UV $\alpha$ parameter transformation only by rephasing, which
innovates the invariance proof of the Hamiltonian. The quantum mechanical
nature of the symmetry dictates the both $\nu$SM and UV variables to transform
jointly, through which the response of the two sectors are related to reveal
their interplay. Thus, the symmetry can serve for a tool for diagnostics,
probing the interrelation between the $\nu$SM and a low-energy description of
new physics.
High-Energy Astrophysical Neutrinos from Cosmic Strings
2206.06377 [abs] [pdf]
[abstract]
by Cyril Creque-Sarbinowski, Jeffrey Hyde, and Marc Kamionkowski.
Cosmic strings that couple to neutrinos may account for a portion of the
high-energy astrophysical neutrino (HEAN) flux seen by IceCube. Here, we
calculate the observed spectrum of neutrinos emitted from a population of
cosmic string loops that contain quasi-cusps, -kinks, or kink-kink collisions.
We consider two broad neutrino emission models: one where these string features
emit a neutrino directly, and one where they emit a scalar particle which then
eventually decays to a neutrino. In either case, the spectrum of cosmic string
neutrinos does not match that of the observed HEAN spectrum. We thus find that
the maximum contribution of cosmic string neutrinos, through these two
scenarios, to be at most $\sim 45$ % of the observed flux. However, we also
find that the presence of cosmic string neutrinos can lead to bumps in the
observed neutrino spectrum. Finally, for each of the models presented, we
present the viable parameter space for neutrino emission.
Impact of late-time neutrino emission on the diffuse supernova neutrino
background
2206.05299 [abs] [pdf]
[abstract]
by Nick Ekanger, [and 3 more]Shunsaku Horiuchi, Kei Kotake, and Kohsuke Sumiyoshi [hide authors].
In the absence of high-statistics supernova neutrino measurements, estimates
of the diffuse supernova neutrino background (DSNB) hinge on the precision of
simulations of core-collapse supernovae. Understanding the cooling phase of
protoneutron star (PNS) evolution ($\gtrsim1\,{\rm s}$ after core bounce) is
crucial, since approximately 50% of the energy liberated by neutrinos is
emitted during the cooling phase. We model the cooling phase with a hybrid
method by combining the neutrino emission predicted by 3D hydrodynamic
simulations with several cooling-phase estimates, including a novel
two-parameter correlation depending on the final baryonic PNS mass and the time
of shock revival. We find that the predicted DSNB event rate at
Super-Kamiokande can vary by a factor of $\sim2-3$ depending on the
cooling-phase treatment. We also find that except for one cooling estimate, the
range in predicted DSNB events is largely driven by the uncertainty in the
neutrino mean energy. With a good understanding of the late-time neutrino
emission, more precise DSNB estimates can be made for the next generation of
DSNB searches.
Energizing gamma ray bursts via $Z^\prime$ mediated neutrino heating
2206.03485 [abs] [pdf]
[abstract]
by Tanmay Kumar Poddar, Srubabati Goswami, and Arvind Kumar Mishra.
The pair annihilation of neutrinos $(\nu\overline{\nu}\rightarrow e^+e^-)$
can energize violent stellar explosions such as gamma ray bursts (GRBs). The
energy in this neutrino heating mechanism can be further enhanced by modifying
the background spacetime over that of Newtonian spacetime. However, one cannot
attain the maximum GRB energy $(\sim 10^{52}~\rm{erg})$ in either the Newtonian
background or Schwarzschild and Hartle-Thorne background. On the other hand,
using modified gravity theories or the Quintessence field as background
geometries, the maximum GRB energy can be reached. In this paper, we consider
extending the standard model by an extra $U(1)_{\rm{B-L}}$ gauge group and
augmenting the energy deposition by neutrino pair annihilation process
including contributions mediated by the $Z^\prime$ gauge boson belonging to
this model. From the observed energy of GRB, we obtain constraints on
$U(1)_{\rm{B-L}}$ gauge coupling in different background spacetimes. We find
that the bounds on gauge coupling in modified gravity theories and quintessence
background are stronger than those coming from the neutrino-electron scattering
experiments in the limit of small gauge boson masses. Future GRB observations
with better accuracy can further strengthen these bounds.
Evaluations of uncertainties in simulations of propagation of
ultrahigh-energy cosmic-ray nuclei derived from microscopic nuclear models
2206.03447 [abs] [pdf]
[abstract]
by E. Kido, [and 7 more]T. Inakura, M. Kimura, N. Kobayashi, S. Nagataki, N. Shimizu, A. Tamii, and Y. Utsuno [hide authors].
Photodisintegration is a main energy loss process for ultrahigh-energy
cosmic-ray (UHECR) nuclei in intergalactic space. Therefore, it is crucial to
understand systematic uncertainty in photodisintegration when simulating the
propagation of UHECR nuclei. In this work, we calculated the cross sections
using the random phase approximation (RPA) of density functional theory (DFT),
a microscopic nuclear model. We calculated the $E1$ strength of 29 nuclei using
three different density functionals. We obtained the cross sections of
photonuclear reactions, including photodisintegration, with the $E1$ strength.
Then, we implemented the cross sections in the cosmic-ray propagation code
CRPropa. We found that assuming certain astrophysical parameter values, the
difference between UHECR energy spectrum predictions using the RPA calculation
and the default photodisintegration model in CRPropa can be more than the
statistical uncertainty of the spectrum. We also found that the differences
between the RPA calculations and CRPropa default in certain astrophysical
parameters obtained by a combined fit of UHECR energy spectrum and composition
data assuming a phenomenological model of UHECR sources can be more than the
uncertainty of the data.
Non-Standard Interaction of atmospheric neutrino in future experiments
2206.02594 [abs] [pdf]
[abstract]
by Pouya Bakhti, Meshkat Rajaee, and Seodong Shin.
We show the prospects of probing neutral-current non-standard interaction
(NSI) in the propagation of atmospheric neutrinos in future large-volume
neutrino experiments including DUNE, HK, KNO, and ORCA. For DUNE, we utilize
its ability of identifying the tau neutrino event and combine the $\nu_\tau$
appearance with the $\nu_\mu$ disappearance. Based on our simulated results,
the ten years of data taking of the atmospheric neutrinos can enormously
improve the bounds on the NSI parameters $\varepsilon_{\mu \tau}, |
\varepsilon_{\mu \mu} - \varepsilon_{\tau \tau} |$, $\varepsilon_{e \mu }$,
$\varepsilon_{e \tau}$ and $| \varepsilon_{\mu \mu} - \varepsilon_{e e} |$ by a
couple of orders of magnitudes. In addition, we show the expected correlations
between the CP-violation phase $\delta_{CP}$ and the NSI parameters
$\varepsilon_{e\mu}, \varepsilon_{e\tau}$, and $|\varepsilon_{ee} -
\varepsilon_{\mu \mu}|$ and confirm the potentials of DUNE, HK, KNO (combined
with HK) in excluding the "No CP violation" hypothesis at 1$\sigma$, 2$\sigma$,
and 3$\sigma$, respectively.
Concept for a Space-based Near-Solar Neutrino Detector
2206.00703 [abs] [pdf]
[abstract]
by N. Solomey, [and 10 more]J. Folkerts, H. Meyer, C. Gimar, J. Novak, B. Doty, T. English, L. Buchele, A. Nelsen, R. McTaggart, and M. Christl [hide authors].
The concept of putting a neutrino detector in close orbit of the sun has been
unexplored until very recently. The primary scientific return is to vastly
enhance our understanding of the solar interior, which is a major NASA goal.
Preliminary calculations show that such a spacecraft, if properly shielded, can
operate in space environments while taking data from neutrino interactions.
These interactions can be distinguished from random background rates of solar
electromagnetic emissions, galactic charged cosmic-rays, and gamma-rays by
using a double pulsed signature. Early simulations of this project have shown
this veto schema to be successful in eliminating background and identifying the
neutrino interaction signal in upwards of 75% of gamma ray interactions and
nearly 100% of other interactions. Hence, we propose a new instrument to
explore and study our sun. Due to inverse square scaling, this instrument has
the potential to outperform earth-based experiments in several domains such as
making measurements not accessible from the earth's orbit.
May 2022
Abundances of uranium and thorium elements in Earth estimated by
geoneutrino spectroscopy
2205.14934 [abs] [pdf]
[abstract]
by S. Abe, [and 67 more]S. Asami, M. Eizuka, S. Futagi, A. Gando, Y. Gando, T. Gima, A. Goto, T. Hachiya, K. Hata, K. Hosokawa, K. Ichimura, S. Ieki, H. Ikeda, K. Inoue, K. Ishidoshiro, Y. Kamei, N. Kawada, Y. Kishimoto, M. Koga, M. Kurasawa, N. Maemura, T. Mitsui, H. Miyake, T. Nakahata, K. Nakamura, K. Nakamura, R. Nakamura, H. Ozaki, T. Sakai, H. Sambonsugi, I. Shimizu, Y. Shirahata, J. Shirai, K. Shiraishi, A. Suzuki, Y. Suzuki, A. Takeuchi, K. Tamae, H. Watanabe, Y. Yoshida, S. Obara, A. K. Ichikawa, S. Yoshida, S. Umehara, K. Fushimi, K. Kotera, Y. Urano, B. E. Berger, B. K. Fujikawa, J. G. Learned, J. Maricic, S. N. Axani, Z. Fu, J. Smolsky, L. A. Winslow, Y. Efremenko, H. J. Karwowski, D. M. Markoff, W. Tornow, A. Li, J. A. Detwiler, S. Enomoto, M. P. Decowski, C. Grant, H. Song, T. O'Donnell, and S. Dell'Oro [hide authors].
The decay of the primordial isotopes $^{238}\mathrm{U}$, $^{235}\mathrm{U}$,
$^{232}\mathrm{Th}$, and $^{40}\mathrm{K}$ have contributed to the terrestrial
heat budget throughout the Earth's history. Hence the individual abundance of
those isotopes are key parameters in reconstructing contemporary Earth model.
The geoneutrinos produced by the radioactive decays of uranium and thorium have
been observed with the Kamioka Liquid-Scintillator Antineutrino Detector
(KamLAND). Those measurements have been improved with more than 18-year
observation time, and improvements in detector background levels mainly by an
8-year almost rector-free period now permit spectroscopy with geoneutrinos. Our
results yield the first constraint on both uranium and thorium heat
contributions. Herein the KamLAND result is consistent with geochemical
estimations based on elemental abundances of chondritic meteorites and mantle
peridotites. The High-Q model is disfavored at 99.76% C.L. and a fully
radiogenic model is excluded at 5.2$\sigma$ assuming a homogeneous heat
producing element distribution in the mantle.
Dark Matter Pollution in the Diffuse Supernova Neutrino Background
2205.14123 [abs] [pdf]
[abstract]
by Nicole F. Bell, Matthew J. Dolan, and Sandra Robles.
The Hyper-Kamiokande (HyperK) experiment is expected to precisely measure the
Diffuse Supernova Neutrino Background (DSNB). This requires that the
backgrounds in the relevant energy range are well understood. One possible
background that has not been considered thus far is the annihilation of
low-mass dark matter (DM) to neutrinos. We conduct simulations of the DSNB
signal and backgrounds in HyperK, and quantify the extent to which DM
annihilation products can pollute the DSNB signal. We find that the presence of
DM could affect the determination of the correct values of parameters of
interest for DSNB physics, such as effective neutrino temperatures and star
formation rates. While this opens the possibility of simultaneously
characterising the DNSB and discovering dark matter via indirect detection, we
argue that it would be hard to disentangle the two contributions due to the
lack of angular information available at low energies.
Determination of supermassive black hole spins in local active galactic
nuclei
2205.10623 [abs] [pdf]
[abstract]
by M. Yu. Piotrovich, S. D. Buliga, and T. M. Natsvlishvili.
We estimated the radiative efficiency and spin value for a number of local
active galactic nuclei with z < 0.34 using 3 popular models connecting the
radiative efficiency with such parameters of AGNs as mass of supermassive black
hole, angle between the line of sight and the axis of the accretion disk and
bolometric luminosity. Analysis of the obtained data shown that the spin value
decreases with cosmic time, which is in agreement with results of theoretical
calculations for low redshift AGNs of other authors. Also we found that the
spin value increases with the increasing mass of SMBH and bolometric
luminosity. This is the expected result that corresponds to theoretical
calculations. Analysis of the distribution of the spin values shown a
pronounced peak in the distribution in 0.75 < a < 1.0 range. ~ 40% of objects
have spin a > 0.75 and ~ 50% of objects have spin a > 0.5. This results are in
a good agreement with our previous results and with the results of other
authors.
Termination of Superradiance from a Binary Companion
2205.10527 [abs] [pdf]
[abstract]
by Xi Tong, Yi Wang, and Hui-Yu Zhu.
We study the impact of a binary companion on black hole superradiance at
orbital frequencies away from the gravitational-collider-physics (GCP)
resonance bands. A superradiant state can couple to a strongly absorptive state
via the tidal perturbation of the companion, thereby acquiring a suppressed
superradiance rate. Below a critical binary separation, this superradiance rate
becomes negative, and the boson cloud gets absorbed by the black hole. This
critical binary separation leads to tight constraints on GCP. Especially, a
companion with mass ratio $q>10^{-3}$ invalidates all GCP fine structure
transitions, as well as almost all Bohr transitions except those from the
$|\psi_{211}\rangle$ state. Meanwhile, the backreaction on the companion
manifests itself as a torque acting on the binary, producing floating/sinking
orbits that can be verified via pulsar timing. In addition, the possible
termination of cloud growth may help to alleviate the current bounds on the
ultralight boson mass from various null detections.
Parametric resonance in neutrino oscillations induced by ultra-light
dark matter and implications for KamLAND and JUNO
2205.09769 [abs] [pdf]
[abstract]
by Marta Losada, [and 4 more]Yosef Nir, Gilad Perez, Inbar Savoray, and Yogev Shpilman [hide authors].
If ultra-light dark matter (ULDM) exists and couples to neutrinos, the
neutrino oscillation probability might be significantly altered by a parametric
resonance. This resonance can occur if the typical frequency of neutrino
flavor-oscillations $\Delta m^2/(2E)$, where $\Delta m^2$ is the mass-squared
difference of the neutrinos and $E$ is the neutrino energy, matches the
oscillation frequency of the ULDM field, determined by its mass, $m_\phi$. The
resonance could lead to observable effects even if the ULDM coupling is very
small, and even if its typical oscillation period, given by
$\tau_\phi=2\pi/m_\phi$, is much shorter than the experimental temporal
resolution. Defining a small parameter $\epsilon_\phi$ to be the ratio between
the contribution of the ULDM field to the neutrino mass and the vacuum value of
the neutrino mass, the impact of the resonance is particularly significant if
$\epsilon_\phi m_\phi L\gtrsim 4$, where $L$ is the distance between the
neutrino source and the detector. Such parametric resonance can improve the fit
to the KamLAND experiment measurements by about $3.5\,\sigma$ compared to
standard oscillations. This scenario will be tested by the JUNO experiment.
Detector Requirements for Model-Independent Measurements of Ultrahigh
Energy Neutrino Cross Sections
2205.09763 [abs] [pdf]
[abstract]
by Ivan Esteban, Steven Prohira, and John F. Beacom.
The ultrahigh energy range of neutrino physics (above $\sim 10^{7} \,
\mathrm{GeV}$), as yet devoid of detections, is an open landscape with
challenges to be met and discoveries to be made. Neutrino-nucleon cross
sections in that range - with center-of-momentum energies $\sqrt{s} \gtrsim 4
\, \mathrm{TeV}$ - are powerful probes of unexplored phenomena. We present a
simple and accurate model-independent framework to evaluate how well these
cross sections can be measured for an unknown flux and generic detectors. We
also demonstrate how to characterize and compare detector sensitivity. We show
that cross sections can be measured to $\simeq ^{+65}_{-30}$% precision over
$\sqrt{s} \simeq$ 4-140 TeV ($E_\nu = 10^7$-$10^{10}$ GeV) with modest energy
and angular resolution and $\simeq 10$ events per energy decade. Many allowed
novel-physics models (extra dimensions, leptoquarks, etc.) produce much larger
effects. In the distant future, with $\simeq 100$ events at the highest
energies, the precision would be $\simeq 15\%$, probing even QCD saturation
effects.
Non-Universal Stellar Initial Mass Functions: Large Uncertainties in
Star Formation Rates at $z\approx 2-4$ and Other Astrophysical Probes
2205.07845 [abs] [pdf]
[abstract]
by Joshua J. Ziegler, [and 6 more]Thomas D. P. Edwards, Anna M. Suliga, Irene Tamborra, Shunsaku Horiuchi, Shin'ichiro Ando, and Katherine Freese [hide authors].
We explore the assumption, widely used in many astrophysical calculations,
that the stellar initial mass function (IMF) is universal across all galaxies.
By considering both a canonical Salpeter-like IMF and a non-universal IMF, we
are able to compare the effect of different IMFs on multiple observables and
derived quantities in astrophysics. Specifically, we consider a non-universal
IMF which varies as a function of the local star formation rate, and explore
the effects on the star formation rate density (SFRD), the extragalactic
background light, the supernova (both core-collapse and thermonuclear) rates,
and the diffuse supernova neutrino background. Our most interesting result is
that our adopted varying IMF leads to much greater uncertainty on the SFRD at
$z \approx 2-4$ than is usually assumed. Indeed, we find a SFRD (inferred using
observed galaxy luminosity distributions) that is a factor of $\gtrsim 3$ lower
than canonical results obtained using a universal Salpeter-like IMF. Secondly,
the non-universal IMF we explore implies a reduction in the supernova
core-collapse rate of a factor of $\sim2$, compared against a universal IMF.
The other potential tracers are only slightly affected by changes to the
properties of the IMF. We find that currently available data do not provide a
clear preference for universal or non-universal IMF. However, improvements to
measurements of the star formation rate and core-collapse supernova rate at
redshifts $z \gtrsim 2$ may offer the best prospects for discernment.
Constraining super-light sterile neutrinos at Borexino and KamLAND
2205.07574 [abs] [pdf]
[abstract]
by Zikang Chen, [and 3 more]Jiajun Liao, Jiajie Ling, and Baobiao Yue [hide authors].
The presence of a super-light sterile neutrino can lead to a dip in the
survival probability of solar neutrinos, and explain the suppression of the
upturn in the low energy solar neutrino data. In this work, we systematically
study the survival probabilities in the 3+1 framework by taking into account of
the non-adiabatic transitions and the coherence effect. We obtain an analytic
equation that can predict the position of the dip. We also place constraints on
the parameter space of sterile neutrinos by using the latest Borexino and
KamLAND data. We find that the low and high energy neutrino data at Borexino
are sensitive to different regions in the sterile neutrino parameter space. In
the case with only $\theta_{01}$ being nonzero, the $\rm{{}^{8}B}$ data sets
the strongest bounds at $\Delta m_{01}^{2} \approx (1.1\sim2.2)\Delta
m_{21}^{2}$, while the low energy neutrino data is more sensitive to other
mass-squared regions. The lowest bounds on $\Delta m_{01}^{2}$ from the
$\rm{pp}$ data can reach $10^{-12} \ \rm{eV^{2}}$ because of the coherence
effect. Also, due to the presence of non-adiabatic transitions, the bounds in
the range of $10^{-9} \ \textrm{eV}^{2} \lesssim \Delta m_{01}^{2} \lesssim
10^{-5} \ \textrm{eV}^{2}$ become weaker as $\Delta m_{01}^{2}$ or
$\sin^{2}2\theta_{01}$ decreases. We also find that in the case with only
$\theta_{02}$ or $\theta_{03}$ being nonzero, the low energy solar neutrino
data set similar but weaker bounds as compared to the case with only
$\theta_{01}$ being nonzero. However, the bounds from the high energy solar
data and the KamLAND data are largely affected by the sterile mixing angles.
Constraining Feeble Neutrino Interactions with Ultralight Dark Matter
2205.06821 [abs] [pdf]
[abstract]
by Abhish Dev, [and 3 more]Gordan Krnjaic, Pedro Machado, and Harikrishnan Ramani [hide authors].
If ultralight $(\ll$ eV), bosonic dark matter couples to right handed
neutrinos, active neutrino masses and mixing angles depend on the ambient dark
matter density. When the neutrino Majorana mass, induced by the dark matter
background, is small compared to the Dirac mass, neutrinos are "pseudo-Dirac"
fermions that undergo oscillations between nearly degenerate active and sterile
states.
We present a complete cosmological history for such a scenario and find
severe limits from a variety of terrestrial and cosmological observables. For
scalar masses in the "fuzzy" dark matter regime ($\sim 10^{-20}$ eV), these
limits exclude couplings of order $10^{-30}$, corresponding to Yukawa
interactions comparable to the gravitational force between neutrinos and
surpassing equivalent limits on time variation in scalar-induced electron and
proton couplings.
Constraining Fundamental Constant Variations from Ultralight Dark Matter
with Pulsar Timing Arrays
2205.06817 [abs] [pdf]
[abstract]
by David E. Kaplan, Andrea Mitridate, and Tanner Trickle.
Pulsar Timing Arrays (PTAs) are exceptionally sensitive detectors in the
frequency band $\text{nHz} \lesssim f \lesssim \mu\text{Hz}$. Ultralight dark
matter (ULDM), with mass in the range $10^{-23}\,\text{eV} \lesssim m_\phi
\lesssim 10^{-20}\,\text{eV}$, is one class of DM models known to generate
signals in this frequency window. While purely gravitational signatures of ULDM
have been studied previously, in this work we consider two signals in PTAs
which arise in presence of direct couplings between ULDM and ordinary matter.
These couplings induce variations in fundamental constants, i.e., particle
masses and couplings. These variations can alter the moment of inertia of
pulsars, inducing pulsar spin fluctuations via conservation of angular
momentum, or induce apparent timing residuals due to reference clock shifts. By
using mock data mimicking current PTA datasets, we show that PTA experiments
outperform torsion balance and atomic clock constraints for ULDM coupled to
electrons, muons, or gluons. In the case of coupling to quarks or photons, we
find that PTAs and atomic clocks set similar constraints. Additionally, we
discuss how future PTAs can further improve these constraints, and detail the
unique properties of these signals relative to the previously studied effects
of ULDM on PTAs.
Superradiant evolution of the shadow and photon ring of Sgr A$^\star$
2205.06238 [abs] [pdf]
[abstract]
by Yifan Chen, [and 3 more]Rittick Roy, Sunny Vagnozzi, and Luca Visinelli [hide authors].
Ultralight bosons can affect the dynamics of spinning black holes (BHs) via
superradiant instability, which can lead to a time evolution of the
supermassive BH shadow. We study prospects for witnessing the
superradiance-induced BH shadow evolution, considering ultralight vector and
tensor fields. We introduce two observables sensitive to the shadow
time-evolution: the shadow drift, and the variation in the azimuthal angle
lapse associated to the photon ring autocorrelation. The two observables are
shown to be highly complementary, depending on the observer's inclination
angle. Focusing on the supermassive object Sgr A$^\star$ we show that both
observables can vary appreciably over human timescales of a few years in the
presence of superradiant instability, leading to signatures which are well
within the reach of the Event Horizon Telescope for realistic observation times
(but benefiting significantly from extended observation periods), and paving
the way towards probing ultralight bosons in the $\sim 10^{-17}\,{\rm eV}$ mass
range.
Core-passing atmospheric neutrinos: a unique probe to discriminate
between Lorentz violation and non-standard interactions
2205.05134 [abs] [pdf]
[abstract]
by Sadashiv Sahoo, [and 3 more]Anil Kumar, Sanjib Kumar Agarwalla, and Amol Dighe [hide authors].
Lorentz violation and non-standard interactions are two of the most popular
scenarios beyond the Standard Model of particle physics, both of which can
affect neutrino oscillations significantly. However, these effects can mimic
each other, and it would be difficult to distinguish between them in any
fixed-baseline neutrino experiment. We show that atmospheric neutrinos, having
access to a wide range of baselines, can break this degeneracy. Observations of
core-passing atmospheric neutrinos and antineutrinos would be a potent tool to
discriminate between these two new-physics scenarios.
First results of the nuGeN experiment on coherent elastic
neutrino-nucleus scattering
2205.04305 [abs] [pdf]
[abstract]
by I. Alekseev, [and 23 more]K. Balej, V. Belov, S. Evseev, D. Filosofov, M. Fomina, Z. Hons, D. Karaivanov, S. Kazartsev, J. Khushvaktov, A. Kuznetsov, A. Lubashevskiy, D. Medvedev, D. Ponomarev, A. Rakhimov, K. Shakhov, E. Shevchik, M. Shirchenko, K. Smolek, S. Rozov, I. Rozova, S. Vasilyev, E. Yakushev, and I. Zhitnikov [hide authors].
The nuGeN experiment is aimed to investigate neutrino properties using
antineutrinos from the reactor of the Kalinin Nuclear Power Plant. The
experimental setup is located at about 11 meters from the center of the 3.1
GWth reactor core. Scattering of the antineutrinos from the reactor is detected
with low energy threshold high purity germanium detector. Passive and active
shieldings are used to suppress all kinds of backgrounds coming from
surrounding materials and cosmic radiation. The description of the experimental
setup together with the first results is presented. The data taken in regimes
with reactor ON (94.50 days) and reactor OFF (47.09 days) have been compared.
No significant difference between spectra of two data sets is observed, i.e. no
positive signals for coherent elastic neutrino-nucleus scattering are detected.
Under Standard Model assumptions about coherent neutrino scattering an upper
limit on a quenching parameter k < 0.26 (90 \% C.L.) in germanium has been set.
Vector leptoquark $U_3$ and CP violation at T2K, NOvA experiments
2205.04269 [abs] [pdf]
[abstract]
by Rudra Majhi, [and 3 more]Dinesh Kumar Singha, K. N. Deepthi, and Rukmani Mohanta [hide authors].
In the current epoch of neutrino physics, many experiments are aiming for
precision measurements of oscillation parameters. Thus, various new physics
scenarios which alter the neutrino oscillation probabilities in matter deserve
careful investigation. In this context, we study the effect of a vector
leptoquark which induces non-standard neutrino interactions (NSI) that modify
the oscillation probabilities of neutrinos in matter. We show that such
interactions provide a relatively large value of NSI parameter $\varepsilon_{e
\mu}$. Considering this NSI parameter, we successfully explain the recent
discrepancy between the observed $\delta_{CP}$ results of T2K and NOvA.
Multi-messenger High-Energy Signatures of Decaying Dark Matter and the
Effect of Background Light
2205.03416 [abs] [pdf]
[abstract]
by Barbara Skrzypek, Marco Chianese, and Carlos Argüelles Delgado.
The IceCube Neutrino Observatory at the South Pole has measured astrophysical
neutrinos using through-going and starting events in the TeV to PeV energy
range. The origin of these astrophysical neutrinos is still largely unresolved,
and among their potential sources could be dark matter decay. Measurements of
the astrophysical flux using muon neutrinos are in slight tension with starting
event measurements. This tension is driven by an excess observed in the energy
range of 40-200 TeV with respect to the through-going expectation. Previous
works have considered the possibility that this excess may be due to heavy dark
matter decay and have placed constraints using gamma-ray and neutrino data.
However, these constraints are not without caveats since they rely on the
modeling of the astrophysical neutrino flux and the sources of gamma-ray
emission. In this work, we derive background-agnostic galactic and
extragalactic constraints on decaying dark matter by considering Tibet
AS$_\gamma$ data, Fermi-LAT diffuse data, and the IceCube high-energy starting
event sample. For the gamma-ray limits, we investigate the uncertainties on
secondary emission from electromagnetic cascades during propagation arising
from the unknown intensity of the extragalactic background light. We find that
such uncertainties amount to a variation of up to $\sim 55\%$ in the gamma-ray
limits derived with extragalactic data. Our results imply that a significant
fraction of the astrophysical neutrino flux could be due to dark matter and
that ruling it out depends on the assumptions on the gamma-ray and neutrino
background. The latter depends on the yet unidentified sources.
Matter effects on flavor transitions of high-energy astrophysical
neutrinos based on different decoherence schemes
2205.03164 [abs] [pdf]
[abstract]
by Ding-Hui Xu and Shu-Jun Rong.
The progress of neutrino astronomy makes the precise measurement of the
flavor ratio of high energy astronomical neutrinos (HANs) possible in the near
future. Then matter effects and new physics effects on the flavor transition of
HANs could be tested by the next-generation neutrino telescopes. In this paper
we study matter effects in gas around the sources of HANs. The matter effects
are dependent on both the decoherence schemes and the sources of neutrinos. We
examine the predictions on the flavor ratio at Earth for typical sources with
five decoherence schemes. For the adiabatic schemes, the matter effect is
notable and may be identified in the special range of the electron density,
irrespective of the production sources of HANs. Hence, the precise measurement
of the flavor ratio would provide constrains on the propagation schemes and the
matter parameter.
Confronting the prediction of leptonic Dirac CP-violating phase with
experiments
2205.02796 [abs] [pdf]
[abstract]
by Yang Hwan Ahn, [and 3 more]Sin Kyu Kang, Raymundo Ramos, and Morimitsu Tanimoto [hide authors].
We update and improve past efforts to predict the leptonic Dirac CP-violating
phase with models that predict perturbatively modified tribimaximal or
bimaximal mixing. Simple perturbations are applied to both mixing patterns in
the form of rotations between two sectors. By translating these perturbed
mixing matrices to the standard parameterization for the neutrino mixing matrix
we derive relations between the Dirac CP-phase and the oscillation angles. We
use these relations together with current experimental results to constrain the
allowed range for the CP-phase and determine its probability density.
Furthermore, we elaborate on the prospects for future experiments probing on
the perturbations considered in this work. We present a model with $A_4$
modular symmetry that is consistent with one of the described perturbed
scenarios and successfully predicts current oscillation parameter data.
Neutrino mass and mass ordering: No conclusive evidence for normal
ordering
2205.02195 [abs] [pdf]
[abstract]
by Stefano Gariazzo, [and 10 more]Martina Gerbino, Thejs Brinckmann, Massimiliano Lattanzi, Olga Mena, Thomas Schwetz, Shouvik Roy Choudhury, Katherine Freese, Steen Hannestad, Christoph A. Ternes, and Mariam Tórtola [hide authors].
The extraction of the neutrino mass ordering is one of the major challenges
in particle physics and cosmology, not only for its implications for a
fundamental theory of mass generation in nature, but also for its decisive role
in the scale of future neutrinoless double beta decay experimental searches. It
has been recently claimed that current oscillation, beta decay and cosmological
limits on the different observables describing the neutrino mass parameter
space provide robust decisive Bayesian evidence in favor of the normal ordering
of the neutrino mass spectrum [arXiv:2203.14247]. We further investigate these
strong claims using a rich and wide phenomenology, with different sampling
techniques of the neutrino parameter space. Contrary to the findings of Jimenez
et al [arXiv:2203.14247], no decisive evidence for the normal mass ordering is
found. Neutrino mass ordering analyses must rely on priors and
parameterizations that are ordering-agnostic: robust results should be regarded
as those in which the preference for the normal neutrino mass ordering is
driven exclusively by the data, while we find a difference of up to a factor of
33 in the Bayes factors among the different priors and parameterizations
exploited here. An ordering-agnostic prior would be represented by the case of
parameterizations sampling over the two mass splittings and a mass scale, or
those sampling over the individual neutrino masses via normal prior
distributions only. In this regard, we show that the current significance in
favor of the normal mass ordering should be taken as $2.7\sigma$ (i.e. moderate
evidence), mostly driven by neutrino oscillation data.
The diffuse supernova neutrino background as a probe of late-time
neutrino mass generation
2205.01102 [abs] [pdf]
[abstract]
by André de Gouvêa, [and 3 more]Ivan Martinez-Soler, Yuber F. Perez-Gonzalez, and Manibrata Sen [hide authors].
The relic neutrinos from old supernova explosions are among the most ancient
neutrino fluxes within experimental reach. Thus, the diffuse supernova neutrino
background (DSNB) could teach us if neutrino masses were different in the past
(redshifts $z\lesssim 5$). Oscillations inside the supernova depend strongly on
the neutrino mass-squared differences and the values of the mixing angles,
rendering the DSNB energy spectrum sensitive to variations of these parameters.
Considering a purely phenomenological parameterization of the neutrino masses
as a function of redshift, we compute the expected local DSNB spectrum here on
Earth. Given the current knowledge of neutrino oscillation parameters,
specially the fact that $|U_{e3}|^2$ is small, we find that the $\nu_e$
spectrum could be significantly different from standard expectations if
neutrinos were effectively massless at $z\gtrsim1$ as long as the neutrino mass
ordering is normal. On the other hand, the $\overline{\nu}_e$ flux is not
expected to be significantly impacted. Hence, a measurement of both the
neutrino and antineutrino components of the DSNB should allow one to test the
possibility of recent neutrino mass generation.
April 2022
Compatibility of Neutrino DIS Data and Its Impact on Nuclear Parton
Distribution Functions
2204.13157 [abs] [pdf]
[abstract]
by K. F. Muzakka, [and 11 more]P. Duwentäster, T. J. Hobbs, T. Ježo, M. Klasen, K. Kovařík, A. Kusina, J. G. Morfín, F. I. Olness, R. Ruiz, I. Schienbein, and J. Y. Yu [hide authors].
In global analyses of nuclear parton distribution functions (nPDFs), neutrino
deep-inelastic scattering (DIS) data have been argued to exhibit tensions with
the data from charged-lepton DIS. Using the nCTEQ framework, we investigate
these possible tensions both internally and with the data sets used in our
recent nPDF analysis nCTEQ15WZSIH. We take into account nuclear effects in the
calculation of the deuteron structure function $F_2^D$ using the CJ15 analysis.
The resulting nPDF fit, nCTEQ15WZSIHdeut, serves as the basis for our
comparison with inclusive neutrino DIS and charm dimuon production data. Using
$\chi^2$ hypothesis testing, we confirm evidence of tensions with these data
and study the impact of the proton PDF baseline as well as the treatment of
data correlation and normalization uncertainties. We identify the experimental
data and kinematic regions that generate the tensions and present several
possible approaches how a consistent global analysis with neutrino data can be
performed. We show that the tension can be relieved using a kinematic cut at
low $x$ ($x>0.1$) and also investigate a possibility of managing the tensions
by using uncorrelated systematic errors. Finally, we present a different
approach identifying a subset of neutrino data which leads to a consistent
global analysis without any additional cuts. Understanding these tensions
between the neutrino and charged-lepton DIS data is important not only for a
better flavor separation in global analyses of nuclear and proton PDFs, but
also for neutrino physics and for searches for physics beyond the Standard
Model.
Timing and Multi-Channel: Novel Method for Determining the Neutrino Mass
Ordering from Supernovae
2204.13135 [abs] [pdf]
[abstract]
by Vedran Brdar and Xun-Jie Xu.
One of the few remaining unknowns in the standard three-flavor neutrino
oscillation paradigm is the ordering of neutrino masses. In this work we
propose a novel method for determining neutrino mass ordering using the time
information on early supernova neutrino events. In a core-collapse supernova,
neutrinos are produced earlier than antineutrinos and, depending on the mass
ordering which affects the adiabatic flavor evolution, may cause earlier
observable signals in $\nu_e$ detection channels than in others. Hence, the
time differences are sensitive to the mass ordering. We find that using the
time information on the detection of the first galactic supernova events at
future detectors like DUNE, JUNO and Hyper-Kamiokande, the mass ordering can
already be determined at $\sim 2 \sigma$ CL, while $\mathcal{O}(10)$ events
suffice for the discovery. Our method does not require high statistics and
could be used within the supernova early warning system (SNEWS) which will have
access to the time information on early supernova neutrino events recorded in a
number of detectors. The method proposed in this paper also implies a crucial
interplay between the mass ordering and the triangulation method for locating
supernovae.
Antineutrino sensitivity at THEIA
2204.12278 [abs] [pdf]
[abstract]
by Stephane Zsoldos, [and 4 more]Zara Bagdasarian, Gabriel D. Orebi Gann, Andrew Barna, and Stephen Dye [hide authors].
We present the sensitivity of the Theia experiment to low-energy geo- and
reactor antineutrinos. For this study, we consider one of the possible proposed
designs, a 17.8-ktonne fiducial volume Theia-25 detector filled with
water-based liquid scintillator placed at Sanford Underground Research Facility
(SURF). We demonstrate Theia's sensitivity to measure the geo- and reactor
antineutrinos via Inverse-Beta Decay interactions after one year of data taking
with $11.9\times10^{32}$ free target protons. The expected number of detected
geo- and reactor antineutrinos is $218\,^{+28}_{-20}$ and $170\,^{+24}_{-20}$,
respectively. The precision of the fitting procedure has been evaluated to be
6.72% and 8.55% for geo- and reactor antineutrinos, respectively. We also
demonstrate the sensitivity towards fitting individual Th and U contributions,
with best fit values of $N_\text{Th}=39\,^{+18}_{-15}$ and
$N_\text{U}=180\,^{+26}_{-22}$. We obtain $(\text{Th}/\text{U})=4.3\pm2.6$
after one year of data taking, and within ten years, the relative precision of
the (Th/U) mass ratio will be reduced to 15%. Finally, from the fit results of
individual Th and U contributions, we evaluate the mantle signal to be
$S_\text{mantle} = 9.0\,\pm [4.2,4.5]$NIU. This was obtained assuming a
full-range positive correlation ($\rho_c\in[0, 1]$) between Th and U, and the
projected uncertainties on the crust contributions of 8.3% (Th) and 7.0% (U).
When considering systematic uncertainties on the signal and background shape
and fluxes, the mantle signal becomes $S_\text{mantle} = 9.3\,\pm
[5.2,5.4]$NIU.
Microscopic and Macroscopic Effects in the Decoherence of Neutrino
Oscillations
2204.10696 [abs] [pdf]
[abstract]
by Ting Cheng, Manfred Lindner, and Werner Rodejohann.
We present a generic structure (the layer structure) for decoherence effects
in neutrino oscillations, which includes decoherence from quantum mechanical
and classical uncertainties. The calculation is done by combining the concept
of open quantum system and quantum field theory, forming a structure composed
of phase spaces from microscopic to macroscopic level. Having information loss
at different levels, quantum mechanical uncertainties parameterize decoherence
by an intrinsic mass eigenstate separation effect, while decoherence for
classical uncertainties is typically dominated by a statistical averaging
effect. With the help of the layer structure, we classify the former as state
decoherence (SD) and the latter as phase decoherence (PD), then further
conclude that both SD and PD result from phase wash-out effects of different
phase structures on different layers. Such effects admit for simple numerical
calculations of decoherence for a given width and shape of uncertainties. While
our structure is generic, so are the uncertainties, nonetheless, a few notable
ones are: the wavepacket size of the external particles, the effective
interaction volume at production and detection, the energy reconstruction model
and the neutrino production profile. Furthermore, we estimate the experimental
sensitivities for SD and PD parameterized by the uncertainty parameters, for
reactor neutrinos and decay-at-rest neutrinos, using a traditional rate
measuring method and a novel phase measuring method.
Very Light Sterile Neutrinos at NOvA and T2K
2204.09130 [abs] [pdf]
[abstract]
by André de Gouvêa, Giancarlo Jusino Sánchez, and Kevin J. Kelly.
Over the last several years, our understanding of neutrino oscillations has
developed significantly due to the long-baseline measurements of muon-neutrino
disappearance and muon-to-electron-neutrino appearance at the T2K and NOvA
experiments. However, when interpreted under the
standard-three-massive-neutrinos paradigm, a tension has emerged between the
two experiments' data. Here, we examine whether this tension can be alleviated
when a fourth, very light neutrino is added to the picture. Specifically, we
focus on the scenario in which this new neutrino has a mass similar to, or even
lighter than, the three mostly-active neutrinos that have been identified to
date. We find that, for some regions of parameter space, the four-neutrino
framework is favored over the three-neutrino one with moderate (a little under
two sigma) significance. Interpreting these results, we provide future outlook
for near-term and long-term experiments if this four-neutrino framework is
indeed true.
New reactor data improves robustness of neutrino mass ordering
determination
2204.09060 [abs] [pdf]
[abstract]
by Peter B. Denton and Julia Gehrlein.
In neutrino oscillation physics numerous exact degeneracies exist under the
name LMA-Dark. These degeneracies make it impossible to determine the sign of
$\Delta m^2_{31}$ known as the atmospheric mass ordering with oscillation
experiments alone in the presence of new neutrino interactions. The combination
of different measurements including multiple oscillation channels and neutrino
scattering experiments lifts some aspects of these degeneracies. In fact,
previous measurements of coherent elastic neutrino nucleus scattering (CEvNS)
by COHERENT already ruled out the LMA-Dark solution for new physics with
mediators heavier than $M_{Z'}\sim50$ MeV while cosmological considerations
disfavor these scenarios for mediators lighter than $M_{Z'}\sim3$ MeV. Here we
leverage new data from the Dresden-II experiment which provides the strongest
bounds on CEvNS with reactor neutrinos to date. We show that this data
completely removes the degeneracies in the $\nu_e$ sector for mediators down to
the MeV scale at which point constraints from the early universe take over.
While the LMA-Dark degeneracy is lifted in the $\nu_e$ sector, it can still be
restored in the $\nu_\mu$ and $\nu_\tau$ sector or with very specific couplings
to up and down quarks, and we speculate on a path forward.
Independent determination of the Earth's orbital parameters with solar
neutrinos in Borexino
2204.07029 [abs] [pdf]
[abstract]
by S. Appel, [and 78 more]Z. Bagdasarian, D. Basilico, G. Bellini, J. Benziger, R. Biondi, B. Caccianiga, F. Calaprice, A. Caminata, A. Chepurnov, D. D'Angelo, A. Derbin, A. Di Giacinto, V. Di Marcello, X. F. Ding, A. Di Ludovico, L. Di Noto, I. Drachnev, D. Franco, C. Galbiati, C. Ghiano, M. Giammarchi, A. Goretti, A. S. Goettel, M. Gromov, D. Guffanti, Aldo Ianni, Andrea Ianni, A. Jany, V. Kobychev, G. Korga, S. Kumaran, M. Laubenstein, E. Litvinovich, P. Lombardi, I. Lomskaya, L. Ludhova, G. Lukyanchenko, I. Machulin, J. Martyn, E. Meroni, L. Miramonti, M. Misiaszek, V. Muratova, R. Nugmanov, L. Oberauer, V. Orekhov, F. Ortica, M. Pallavicini, L. Pelicci, O. Penek, L. Pietrofaccia, N. Pilipenko, A. Pocar, G. Raikov, M. T. Ranalli, G. Ranucci, A. Razeto, A. Re, M. Redchuk, N. Rossi, S. Schoenert, D. Semenov, G. Settanta, M. Skorokhvatov, A. Singhal, O. Smirnov, A. Sotnikov, R. Tartaglia, G. Testera, E. Unzhakov, A. Vishneva, R. B. Vogelaar, F. von Feilitzsch, M. Wojcik, M. Wurm, S. Zavatarelli, K. Zuber, and G. Zuzel [hide authors].
Since the beginning of 2012, the Borexino collaboration has been reporting
precision measurements of the solar neutrino fluxes, emitted in the
proton-proton chain and in the Carbon-Nitrogen-Oxygen cycle. The experimental
sensitivity achieved in Phase-II and Phase-III of the Borexino data taking made
it possible to detect the annual modulation of the solar neutrino interaction
rate due to the eccentricity of Earth's orbit, with a statistical significance
greater than 5$\sigma$. This is the first precise measurement of the Earth's
orbital parameters based solely on solar neutrinos and an additional signature
of the solar origin of the Borexino signal. The complete periodogram of the
time series of the Borexino solar neutrino detection rate is also reported,
exploring frequencies between one cycle/year and one cycle/day. No other
significant modulation frequencies are found. The present results were uniquely
made possible by Borexino's decade-long high-precision solar neutrino
detection.
Analytic treatment of 3-flavor neutrino oscillation and decay in matter
2204.05803 [abs] [pdf]
[abstract]
by Dibya S. Chattopadhyay, [and 3 more]Kaustav Chakraborty, Amol Dighe, and Srubabati Goswami [hide authors].
We present compact analytic expressions for 3-flavor neutrino oscillation
probabilities with invisible neutrino decay, where matter effects have been
explicitly included. We take into account the possibility that the oscillation
and decay components of the effective Hamiltonian do not commute. This is
achieved by employing the techniques of inverse Baker-Campbell-Hausdorff (BCH)
expansion and the Cayley-Hamilton theorem applied in the 3-flavor framework. If
only the vacuum mass eigenstate $\nu_3$ decays, we show that the treatment of
neutrino propagation may be reduced to an effective 2-flavor analysis in the
One Mass Scale Dominance (OMSD) approximation. The oscillation probabilities
for $P_{\mu\mu}$, $P_{ee}$, $P_{e\mu}$ and $P_{\mu e}$ -- relevant for reactor,
long baseline and atmospheric neutrino experiments -- are obtained as
perturbative expansions for the case of only $\nu_3$ decay, as well as for the
more general scenario where all components of the decay matrix are non-zero.
The analytic results thus obtained match the exact numerical results for
constant density matter to a high precision and provide physical insights into
possible effects of the decay of neutrinos as they propagate through Earth
matter. We find that the effects of neutrino decay are most likely to be
observable in $P_{\mu\mu}$. We also point out that at any long baseline, the
oscillation dips in $P_{\mu\mu}$ can show higher survival probabilities in the
case with decay than without decay, and explain this feature using our analytic
approximations.
Exploring the Fate of Stellar Core Collapse with Supernova Relic
Neutrinos
2204.04880 [abs] [pdf]
[abstract]
by Yosuke Ashida and Ken'ichiro Nakazato.
Core collapse of massive stars leads to different fates for various physical
factors, which gives different spectra of the emitted neutrinos. We focus on
the supernova relic neutrinos (SRNs) as a probe to investigate the stellar
collapse fate. We present the SRN fluxes and event rate spectra at a detector
for three resultant states after stellar core collapse, the typical mass
neutron star, the higher mass neutron star, or the failed supernova forming a
black hole, based on different nuclear equations of state. Then possible SRN
fluxes are formed as mixtures of the three components. We also show the
expected sensitivities at the next-generation water-based Cherenkov detectors,
SK-Gd and Hyper-Kamiokande, as constraining the mixture fractions. This study
provides a practical example of extracting astrophysical constraints through
SRN measurement.
Sterile neutrino production at small mixing in the early universe
2204.04224 [abs] [pdf]
[abstract]
by Gonzalo Alonso-Álvarez and James M. Cline.
Sterile neutrinos can be produced in the early universe via interactions with
their active counterparts. For small active-sterile mixing angles, thermal
equilibrium with the standard model plasma is not reached and sterile neutrinos
are only produced via flavor oscillations. We study in detail this regime,
taking into account matter potentials and decoherence effects caused by elastic
scatterings with the plasma. We find that resonant oscillations occurring at
temperatures $T\lesssim 10\,\mathrm{GeV}$ lead to a significant enhancement of
the sterile neutrino production rate. Taking this into account, we improve
constraints on the active-sterile mixing from Big Bang nucleosynthesis and the
cosmic microwave background, excluding mixing angles down to $\theta_s\sim
10^{-10}-10^{-16}$ for sterile neutrino masses in the $10\,\mathrm{MeV}$ to
$10\,\mathrm{GeV}$ range. We observe that if sterile neutrinos predominantly
decay into metastable hidden sector particles, this process provides a novel
dark matter production mechanism, consistent with the sterile neutrino origin
of light neutrino masses via the seesaw mechanism.
Constraining New Physics with Borexino Phase-II spectral data
2204.03011 [abs] [pdf]
[abstract]
by Pilar Coloma, [and 4 more]M. C. Gonzalez-Garcia, Michele Maltoni, João Paulo Pinheiro, and Salvador Urrea [hide authors].
We present a detailed analysis of the spectral data of Borexino Phase II,
with the aim of exploiting its full potential to constrain scenarios beyond the
Standard Model. In particular, we quantify the constraints imposed on neutrino
magnetic moments, neutrino non-standard interactions, and several simplified
models with light scalar, pseudoscalar or vector mediators. Our analysis shows
perfect agreement with those performed by the collaboration on neutrino
magnetic moments and neutrino non-standard interactions in the same restricted
cases and expands beyond those, stressing the interplay between flavour
oscillations and flavour non-diagonal interaction effects for the correct
evaluation of the event rates. For simplified models with light mediators we
show the power of the spectral data to obtain robust limits beyond those
previously estimated in the literature.
Cored Dark Matter halos in the Cosmic Neutrino Background
2204.01431 [abs] [pdf]
[abstract]
by Wonsub Cho, Ki-Young Choi, and Hee Jung Kim.
We study the impact of the interaction between DM and the cosmic neutrino
background on the evolution of galactic dark matter halos. The energy transfer
from the neutrinos to the dark matter can heat the center of the galaxy and
make it cored. This effect is efficient for the small galaxies such as the
satellite galaxies of the Milky Way and we can put conservative constraint on
the non-relativistic elastic scattering cross section as
$\sigma_{\chi\nu}\lesssim 10^{-31} {\rm cm}^2$ for 0.1 keV dark matter and 0.1
eV neutrino.
March 2022
Visible Neutrino Decays and the Impact of the Daughter-Neutrino Mass
2203.14976 [abs] [pdf]
[abstract]
by André de Gouvêa, Manibrata Sen, and Jean Weill.
We compute the differential decay width of two- and three-body neutrino
decays, assuming neutrinos are Dirac fermions and allowing for the possibility
that the decay-daughters have nonzero masses. We examine different hypotheses
for the interaction that mediates neutrino decay and concentrate on identifying
circumstances where the decay-daughters can significantly impact the
neutrino-decay signature at different experiments. We are especially interested
in decay daughters produced by right-chiral neutrino fields, when the mass of
the daughter plays a decisive role. As a concrete example, we compare the
effects of visible and invisible antineutrino decays at the JUNO experimental
setup.
Neutrino Masses and Mass Hierarchy: Evidence for the Normal Hierarchy
2203.14247 [abs] [pdf]
[abstract]
by Raul Jimenez, [and 4 more]Carlos Pena-Garay, Kathleen Short, Fergus Simpson, and Licia Verde [hide authors].
The latest cosmological constraints on the sum of neutrino masses, in
combination with the latest laboratory measurements on oscillations, provide
``decisive" Bayesian evidence for the normal neutrino mass hierarchy. We show
that this result holds across very different prior alternatives by exploring
two extremes on the range of prior choices. In fact, while the specific
numerical value for the Evidence depends on the choice of prior, the Bayesian
odds remain greater than 140:1 across very different prior choices. For
Majorana neutrinos this has important implications for the upper limit of the
neutrino-less double beta decay half life and thus for the technology and
resources needed for future double beta decay experiments.
PeV Tau Neutrinos to Unveil Ultra-High-Energy Sources
2203.13827 [abs] [pdf]
[abstract]
by Carlos A. Argüelles, [and 3 more]Francis Halzen, Ali Kheirandish, and Ibrahim Safa [hide authors].
The observation of ultra-high-energy EeV-energy cosmogenic neutrinos provides
a direct path to identifying the sources of the highest energy cosmic rays;
searches have so far resulted in only upper limits on their flux. However, with
the realization of cubic-kilometer detectors such as IceCube and, in the near
future, KM3NeT, GVD-Baikal, and similar instruments, we anticipate the
observation of PeV-energy cosmic neutrinos with high statistics. In this
context, we draw attention to the opportunity to identify EeV tau neutrinos at
PeV energy using Earth-traversing tau neutrinos. We show that Cherenkov
detectors can improve their sensitivity to transient point sources by more than
an order of magnitude by indirectly observing EeV tau neutrinos with initial
energies that are nominally beyond their reach. This new technique also
improves their sensitivity to the ultra-high-energy diffuse neutrino flux by up
to a factor of two. Our work exemplifies how observing tau neutrinos at PeV
energies provides an unprecedented reach to EeV fluxes.
No CC-NSI explanation of the Gallium anomaly
2203.13659 [abs] [pdf]
[abstract]
by Carlo Giunti and Christoph Andreas Ternes.
We show that the Gallium anomaly can not be explained by CC-NSI.
Rocks, Water and Noble Liquids: Unfolding the Flavor Contents of
Supernova Neutrinos
2203.12696 [abs] [pdf]
[abstract]
by Sebastian Baum, Francesco Capozzi, and Shunsaku Horiuchi.
Measuring core-collapse supernova neutrinos, both from individual supernovae
within the Milky Way and from past core collapses throughout the Universe (the
diffuse supernova neutrino background, or DSNB), is one of the main goals of
current and next generation neutrino experiments. Detecting the heavy-lepton
flavor (muon and tau types, collectively $\nu_x$) component of the flux is
particularly challenging due to small statistics and large backgrounds. While
the next galactic neutrino burst will be observed in a plethora of neutrino
channels, allowing to measure a small number of $\nu_x$ events, only upper
limits are anticipated for the diffuse $\nu_x$ flux even after decades of data
taking with conventional detectors. However, paleo-detectors could measure the
time-integrated flux of neutrinos from galactic core-collapse supernovae via
flavor-blind neutral current interactions. In this work, we show how combining
a measurement of the average galactic core-collapse supernova flux with paleo
detectors and measurements of the DSNB electron-type neutrino fluxes with the
next-generation water Cherenkov detector Hyper-Kamiokande and the liquid noble
gas detector DUNE will allow to determine the mean supernova $\nu_x$ flux
parameters with precision of order ten percent.
Testing Non-Standard Interactions Between Solar Neutrinos and Quarks
with Super-Kamiokande
2203.11772 [abs] [pdf]
[abstract]
by Super-Kamiokande Collaboration, [and 272 more]:, P. Weatherly, K. Abe, C. Bronner, Y. Hayato, K. Hiraide, M. Ikeda, K. Iyogi, J. Kameda, Y. Kanemura, Y. Kataoka, Y. Kato, Y. Kishimoto, S. Miki, M. Miura, S. Moriyama, T. Mochizuki, M. Nakahata, Y. Nakano, S. Nakayama, T. Okada, K. Okamoto, A. Orii, G. Pronost, K. Sato, H. Sekiya, M. Shiozawa, Y. Sonoda, Y. Suzuki, A. Takeda, Y. Takemoto, A. Takenaka, H. Tanaka, S. Tasaka, X. Wang, S. Watanabe, T. Yano, S. Han, T. Kajita, K. Kaneyuki, K. Okumura, T. Tashiro, R. Wang, J. Xia, G. D. Megias, L. Labarga, B. Zaldivar, B. W. Pointon, F. d. M. Blaszczyk, C. Kachulis, E. Kearns, J. L. Raaf, J. L. Stone, L. R. Sulak, S. Sussman, L. Wan, T. Wester, S. Berkman, S. Tobayama, J. Bian, M. Elnimr, N. J. Griskevich, W. R. Kropp, S. Locke, S. Mine, M. B. Smy, H. W. Sobel, V. Takhistov, A. Yankelevich, K. S. Ganezer, J. Hill, J. Y. Kim, I. T. Lim, R. G. Park, B. Bodur, Z. Li, K. Scholberg, C. W. Walter, L. Bernard, A. Coffani, O. Drapier, A. Giampaolo, S. El Hedri, J. Imber, Th. A. Mueller, P. Paganini, B. Quilain, A. D. Santos, T. Ishizuka, T. Nakamura, J. S. Jang, J. G. Learned, S. Matsuno, S. Cao, J. Amey, L. H. V. Anthony, R. P. Litchfield, W. Y. Ma, D. Martin, M. Scott, A. A. Sztuc, Y. Uchida, M. O. Wascko, V. Berardi, M. G. Catanesi, R. A. Intonti, E. Radicioni, N. F. Calabria, L. N. Machado, G. De Rosa, G. Collazuol, F. Iacob, M. Lamoureux, M. Mattiazzi, N. Ospina, L. Ludovici, M. Gonin, Y. Maekawa, Y. Nishimura, M. Friend, T. Hasegawa, T. Ishida, M. Jakkapu, T. Kobayashi, T. Matsubara, T. Nakadaira, K. Nakamura, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, T. Boschi, F. Di Lodovico, J. Gao, T. Katori, J. Migenda, M. Taani, S. Zsoldos, KE. Abe, M. Hasegawa, Y. Isobe, Y. Kotsar, H. Miyabe, H. Ozaki, T. Sugimoto, A. T. Suzuki, Y. Takeuchi, S. Yamamoto, Y. Ashida, J. Feng, T. Hayashino, S. Hirota, M. Jiang, T. Kikawa, M. Mori, T. Nakaya, R. A. Wendell, K. Yasutome, P. Fernandez, N. McCauley, P. Mehta, A. Pritchard, K. M. Tsui, Y. Fukuda, Y. Itow, H. Menjo, M. Murase, K. Frankiewicz, J. Lagoda, S. M. Lakshmi, M. Mandal, P. Mijakowski, Y. S. Prabhu, J. Zalipska, M. Jia, J. Jiang, C. K. Jung, X. Li, J. L. Palomino, G. Santucci, C. Vilela, M. J. Wilking, C. Yanagisawa, D. Fukuda, K. Hagiwara, M. Harada, H. Ishino, S. Ito, H. Kitagawa, Y. Koshio, W. Ma, S. Sakai, M. Sakuda, Y. Takahira, C. Xu, Y. Kuno, G. Barr, D. Barrow, L. Cook, A. Goldsack, S. Samani, C. Simpson, D. Wark, S. Molina Sedgwick, R. Tacik, F. Nova, J. Y. Yang, S. J. Jenkins, M. Malek, J. M. McElwee, O. Stone, M. D. Thiesse, L. F. Thompson, H. Okazawa, Y. Choi, S. B. Kim, J. W. Seo, I. Yu, A. Ichikawa, K. D. Nakamura, K. Nishijima, M. Koshiba, K. Iwamoto, K. Nakagiri, Y. Nakajima, Y. Suda, N. Taniuchi, M. Yokoyama, K. Martens, M. Murdoch, M. R. Vagins, D. Hamabe, S. Izumiyama, M. Kuze, Y. Okajima, T. Yoshida, M. Inomoto, M. Ishitsuka, H. Ito, T. Kinoshita, R. Matsumoto, M. Shinoki, T. Suganuma, M. Yonenaga, J. F. Martin, C. M. Nantais, H. A. Tanaka, T. Towstego, R. Akutsu, P. de Perio, V. Gousy-Leblanc, M. Hartz, A. Konaka, P. de Perio, N. W. Prouse, S. Chen, B. D. Xu, B. Zhang, M. Posiadala-Zezula, D. Hadley, M. Nicholson, M. O'Flaherty, B. Richards, A. Ali, B. Jamieson, P. Giorgio, Ll. Marti, A. Minamino, G. Pintaudi, S. Sano, R. Sasaki, and K. Wada [hide authors].
Non-Standard Interactions (NSI) between neutrinos and matter affect the
neutrino flavor oscillations. Due to the high matter density in the core of the
Sun, solar neutrinos are suited to probe these interactions. Using the $277$
kton-yr exposure of Super-Kamiokande to $^{8}$B solar neutrinos, we search for
the presence of NSI. Our data favors the presence of NSI with down quarks at
1.8$\sigma$, and with up quarks at 1.6$\sigma$, with the best fit NSI
parameters being ($\epsilon_{11}^{d},\epsilon_{12}^{d}$) = (-3.3, -3.1) for
$d$-quarks and ($\epsilon_{11}^{u},\epsilon_{12}^{u}$) = (-2.5, -3.1) for
$u$-quarks. After combining with data from the Sudbury Neutrino Observatory and
Borexino, the significance increases by 0.1$\sigma$.
Snowmass White Paper: Beyond the Standard Model effects on Neutrino
Flavor
2203.10811 [abs] [pdf]
[abstract]
by C. A. Argüelles, [and 25 more]G. Barenboim, M. Bustamante, P. Coloma, P. B. Denton, I. Esteban, Y. Farzan, E. Fernández Martínez, D. V. Forero, A. M. Gago, T. Katori, R. Lehnert, M. Ross-Lonergan, A. M. Suliga, Z. Tabrizi, L. Anchordoqui, K. Chakraborty, J. Conrad, A. Das, C. S. Fong, B. R. Littlejohn, M. Maltoni, D. Parno, J. Spitz, J. Tang, and S. Wissel [hide authors].
Neutrinos are one of the most promising messengers for signals of new physics
Beyond the Standard Model (BSM). On the theoretical side, their elusive nature,
combined with their unknown mass mechanism, seems to indicate that the neutrino
sector is indeed opening a window to new physics. On the experimental side,
several long-standing anomalies have been reported in the past decades,
providing a strong motivation to thoroughly test the standard three-neutrino
oscillation paradigm. In this Snowmass21 white paper, we explore the potential
of current and future neutrino experiments to explore BSM effects on neutrino
flavor during the next decade.
Constraining ultra-high-energy cosmic ray composition through
cross-correlations
2203.09538 [abs] [pdf]
[abstract]
by Konstantinos Tanidis, Federico R. Urban, and Stefano Camera.
The chemical composition of the highest end of the ultra-high-energy cosmic
ray spectrum is very hard to measure experimentally, and to this day it remains
mostly unknown. Since the trajectories of ultra-high-energy cosmic rays are
deflected in the magnetic field of the Galaxy by an angle that depends on their
atomic number $Z$, it could be possible to indirectly measure $Z$ by
quantifying the amount of such magnetic deflections. In this paper we show
that, using the angular harmonic cross-correlation between ultra-high-energy
cosmic rays and galaxies, we could effectively distinguish different atomic
numbers with current data. As an example, we show how, if $Z=1$, the
cross-correlation can exclude a $39\%$ fraction of Fe56 nuclei at $2\sigma$ for
rays above $100\text{EeV}$.
Weaker yet again: mass spectrum-consistent cosmological constraints on
the neutrino lifetime
2203.09075 [abs] [pdf]
[abstract]
by Joe Zhiyu Chen, [and 3 more]Isabel M. Oldengott, Giovanni Pierobon, and Yvonne Y. Y. Wong [hide authors].
We consider invisible neutrino decay $\nu_H \to \nu_l + \phi$ in the
ultra-relativistic limit and compute the neutrino anisotropy loss rate relevant
for the cosmic microwave background (CMB) anisotropies. Improving on our
previous work which assumed massless $\nu_l$ and $\phi$, we reinstate in this
work the daughter neutrino mass $m_{\nu l}$ in a manner consistent with the
experimentally determined neutrino mass splittings. We find that a nonzero
$m_{\nu l}$ introduces a new phase space factor in the loss rate $\Gamma_{\rm
T}$ proportional to $(\Delta m_\nu^2/m_{\nu_H}^2)^2$ in the limit of a small
squared mass gap between the parent and daughter neutrinos, i.e., $\Gamma_{\rm
T} \sim (\Delta m_\nu^2/m_{\nu H}^2)^2 (m_{\nu H}/E_\nu )^5 (1/\tau_0)$, where
$\tau_0$ is the $\nu_H$ rest-frame lifetime. Using a general form of this
result, we update the limit on $\tau_0$ using the Planck 2018 CMB data. We find
that for a parent neutrino of mass $m_{\nu H} \lesssim 0.1 {\rm eV}$, the new
phase space factor weakens the constraint on its lifetime by up to a factor of
50 if $\Delta m_\nu^2$ corresponds to the atmospheric mass gap and up to
$10^{5}$ if the solar mass gap, in comparison with naive estimates that assume
$m_{\nu l}=0$. The revised constraints are (i) $\tau^0 \gtrsim (6 \to 10)
\times 10^5~{\rm s}$ and $\tau^0 \gtrsim (400 \to 500)~{\rm s}$ if only one
neutrino decays to a daughter neutrino separated by, respectively, the
atmospheric and the solar mass gap, and (ii) $\tau^0 \gtrsim (2 \to 3) \times
10^7~{\rm s}$ in the case of two decay channels with one near-common
atmospheric mass gap. In contrast to previous, naive limits which scale as
$m_{\nu H}^5$, these mass spectrum-consistent $\tau_0$ constraints are
remarkably independent of the parent mass and open up a swath of parameter
space within the projected reach of IceCube and other neutrino telescopes in
the next two decades.
Tau Neutrinos in the Next Decade: from GeV to EeV
2203.05591 [abs] [pdf]
[abstract]
by Roshan Mammen Abraham, [and 65 more]Jaime Alvarez-Muñiz, Carlos A. Argüelles, Akitaka Ariga, Tomoko Ariga, Adam Aurisano, Dario Autiero, Mary Bishai, Nilay Bostan, Mauricio Bustamante, Austin Cummings, Valentin Decoene, André de Gouvêa, Giovanni De Lellis, Albert De Roeck, Peter B. Denton, Antonia Di Crescenzo, Milind V. Diwan, Yasaman Farzan, Anatoli Fedynitch, Jonathan L. Feng, Laura J. Fields, Alfonso Garcia, Maria Vittoria Garzelli, Julia Gehrlein, Christian Glaser, Katarzyna Grzelak, Steffen Hallmann, V Hewes, D. Indumathi, Ahmed Ismail, Sudip Jana, Yu Seon Jeong, Kevin J. Kelly, Spencer R. Klein, Felix Kling, Thomas Kosc, Umut Kose, D. Jason Koskinen, John Krizmanic, Jeff Lazar, Yichen Li, Ivan Martinez-Soler, Irina Mocioiu, Jiwoo Nam, Valentin Niess, Nepomuk Otte, Sameer Patel, Roberto Petti, Remy L. Prechelt, Steven Prohira, Miriama Rajaoalisoa, Mary Hall Reno, Ibrahim Safa, Carlos Sarasty-Segura, R. Thiru Senthil, Juliana Stachurska, Oleksandr Tomalak, Sebastian Trojanowski, Roger Alexandre Wendell, Dawn Williams, Stephanie Wissel, Barbara Yaeggy, Enrique Zas, Pavel Zhelnin, and Jing-yu Zhu [hide authors].
Tau neutrinos are the least studied particle in the Standard Model. This
whitepaper discusses the current and expected upcoming status of tau neutrino
physics with attention to the broad experimental and theoretical landscape
spanning long-baseline, beam-dump, collider, and astrophysical experiments.
This whitepaper was prepared as a part of the NuTau2021 Workshop.
Consequences of the Dresden-II reactor data for the weak mixing angle
and new physics
2203.02414 [abs] [pdf]
[abstract]
by D. Aristizabal Sierra, V. De Romeri, and D. K. Papoulias.
The Dresden-II reactor experiment has recently reported a suggestive evidence
for the observation of coherent elastic neutrino-nucleus scattering, using a
germanium detector. Given the low recoil energy threshold, these data are
particularly interesting for a low-energy determination of the weak mixing
angle and for the study of new physics leading to spectral distortions at low
momentum transfer. Using two hypotheses for the quenching factor, we study the
impact of the data on: (i) The weak mixing angle at a renormalization scale of
$\sim 10\,\text{MeV}$, (ii) neutrino generalized interactions with light
mediators, (iii) the sterile neutrino dipole portal. The results for the weak
mixing angle show a strong dependence on the quenching factor choice. Although
still with large uncertainties, the Dresden-II data provide for the first time
a determination of $\sin^2\theta_W$ at such scale using coherent elastic
neutrino-nucleus scattering data. Tight upper limits are placed on the light
vector, scalar and tensor mediator scenarios. Kinematic constraints implied by
the reactor anti-neutrino flux and the ionization energy threshold allow the
sterile neutrino dipole portal to produce up-scattering events with sterile
neutrino masses up to $\sim 8\,$MeV. In this context, we find that limits are
also sensitive to the quenching factor choice, but in both cases competitive
with those derived from XENON1T data and more stringent that those derived with
COHERENT data, in the same sterile neutrino mass range.
Search for the Majorana Nature of Neutrinos in the Inverted Mass
Ordering Region with KamLAND-Zen
2203.02139 [abs] [pdf]
[abstract]
by KamLAND-Zen Collaboration, [and 74 more]:, S. Abe, S. Asami, M. Eizuka, S. Futagi, A. Gando, Y. Gando, T. Gima, A. Goto, T. Hachiya, K. Hata, S. Hayashida, K. Hosokawa, K. Ichimura, S. Ieki, H. Ikeda, K. Inoue, K. Ishidoshiro, Y. Kamei, N. Kawada, Y. Kishimoto, M. Koga, M. Kurasawa, N. Maemura, T. Mitsui, H. Miyake, T. Nakahata, K. Nakamura, K. Nakamura, R. Nakamura, H. Ozaki, T. Sakai, H. Sambonsugi, I. Shimizu, J. Shirai, K. Shiraishi, A. Suzuki, Y. Suzuki, A. Takeuchi, K. Tamae, K. Ueshima, H. Watanabe, Y. Yoshida, S. Obara, A. K. Ichikawa, D. Chernyak, A. Kozlov, K. Z. Nakamura, S. Yoshida, Y. Takemoto, S. Umehara, K. Fushimi, K. Kotera, Y. Urano, B. E. Berger, B. K. Fujikawa, J. G. Learned, J. Maricic, S. N. Axani, J. Smolsky, Z. Fu, L. A. Winslow, Y. Efremenko, H. J. Karwowski, D. M. Markoff, W. Tornow, S. Dell'Oro, T. O'Donnell, J. A. Detwiler, S. Enomoto, M. P. Decowski, C. Grant, A. Li, and H. Song [hide authors].
The KamLAND-Zen experiment has provided stringent constraints on the
neutrinoless double-beta ($0\nu\beta\beta$) decay half-life in $^{136}$Xe using
a xenon-loaded liquid scintillator. We report an improved search using an
upgraded detector with almost double the amount of xenon and an ultralow
radioactivity container, corresponding to an exposure of 970 kg yr of
$^{136}$Xe. These new data provide valuable insight into backgrounds,
especially from cosmic muon spallation of xenon, and have required the use of
novel background rejection techniques. We obtain a lower limit for the
$0\nu\beta\beta$ decay half-life of $T_{1/2}^{0\nu} > 2.3 \times 10^{26}$ yr at
90% C.L., corresponding to upper limits on the effective Majorana neutrino mass
of 36-156 meV using commonly adopted nuclear matrix element calculations.
February 2022
An absolute $ν$ mass measurement with the DUNE experiment
2203.00024 [abs] [pdf]
[abstract]
by Federica Pompa, [and 3 more]Francesco Capozzi, Olga Mena, and Michel Sorel [hide authors].
Time of flight delay in the supernova neutrino signal offers a unique tool to
set model-independent constraints on the absolute neutrino mass. The presence
of a sharp time structure during a first emission phase, the so-called
neutronization burst in the electron neutrino flavor time distribution, makes
this channel a very powerful one. Large liquid argon underground detectors will
provide precision measurements of the time dependence of the electron neutrino
fluxes. We derive here a new $\nu$ mass sensitivity attainable at the future
DUNE far detector from a future supernova collapse in our galactic
neighborhood, finding a sub-eV reach under favorable scenarios. These values
are competitive with those expected for laboratory direct neutrino mass
searches.
Theia: Summary of physics program. Snowmass White Paper Submission
2202.12839 [abs] [pdf]
[abstract]
by M. Askins, [and 86 more]Z. Bagdasarian, N. Barros, E. W. Beier, A. Bernstein, E. Blucher, R. Bonventre, E. Bourret, E. J. Callaghan, J. Caravaca, M. Diwan, S. T. Dye, J. Eisch, A. Elagin, T. Enqvist, U. Fahrendholz, V. Fischer, K. Frankiewicz, C. Grant, D. Guffanti, C. Hagner, A. Hallin, C. M. Jackson, R. Jiang, T. Kaptanoglu, J. R. Klein, Yu. G. Kolomensky, C. Kraus, F. Krennrich, T. Kutter, T. Lachenmaier, B. Land, K. Lande, L. Lebanowski, J. G. Learned, V. A. Li, V. Lozza, L. Ludhova, M. Malek, S. Manecki, J. Maneira, J. Maricic, J. Martyn, A. Mastbaum, C. Mauger, M. Mayer, J. Migenda, F. Moretti, J. Napolitano, B. Naranjo, M. Nieslony, L. Oberauer, G. D. Orebi Gann, J. Ouellet, T. Pershing, S. T. Petcov, L. Pickard, R. Rosero, M. C. Sanchez, J. Sawatzki, S. H. Seo, M. Smiley, M. Smy, A. Stahl, H. Steiger, M. R. Stock, H. Sunej, R. Svoboda, E. Tiras, W. H. Trzaska, M. Tzanov, M. Vagins, C. Vilela, Z. Wang, J. Wang, M. Wetstein, M. J. Wilking, L. Winslow, P. Wittich, B. Wonsak, E. Worcester, M. Wurm, G. Yang, M. Yeh, E. D. Zimmerman, S. Zsoldos, and K. Zuber [hide authors].
Theia would be a novel, "hybrid" optical neutrino detector, with a rich
physics program. This paper is intended to provide a brief overview of the
concepts and physics reach of Theia. Full details can be found in the Theia
white paper [1].
Matter Effects of Sterile Neutrino in Light of Renormalization-Group
Equations
2202.09851 [abs] [pdf]
[abstract]
by Shuge Zeng and Fanrong Xu.
The renormalization-group equation (RGE) approach to neutrino matter effects
is further developed in this work. We derive a complete set of differential
equations for effective mixing elements, masses and Jarlskog-like invariants in
presence of a light sterile neutrino. The evolutions of mixing elements as well
as Jarlskog-like invariants are obtained by numerically solving these
differential equations. We calculate terrestrial matter effects in
long-baseline (LBL) experiments, taking NOvA, T2K and DUNE as examples. In both
three-flavor and four-flavor frameworks, electron-neutrino survival
probabilities as well as the day-night asymmetry of solar neutrino are also
evaluated as a further examination of the RGE approach.
Improving CP Measurement with THEIA and Muon Decay at Rest
2202.05038 [abs] [pdf]
[abstract]
by Shao-Feng Ge, Chui-Fan Kong, and Pedro Pasquini.
We explore the possibility of using the recently proposed THEIA detector to
measure the $\bar \nu_\mu \rightarrow \bar \nu_e$ oscillation with neutrinos
from a muon decay at rest ($\mu$DAR) source to improve the leptonic CP phase
measurement. Due to its intrinsic low-energy beam, this $\mu$THEIA
configuration ($\mu$DAR neutrinos at THEIA) is only sensitive to the genuine
leptonic CP phase $\delta_D$ and not contaminated by the matter effect. With
detailed study of neutrino energy reconstruction and backgrounds at the THEIA
detector, we find that the combination with the high-energy DUNE can
significantly reduce the CP uncertainty, especially around the maximal CP
violation cases $\delta_D = \pm 90^\circ$. Both the $\mu$THEIA-25 with 17kt and
$\mu$THEIA-100 with 70kt fiducial volumes are considered. For DUNE +
$\mu$THEIA-100, the CP uncertainty can be better than $8^\circ$.
Detecting Beyond the Standard Model Interactions of Solar Neutrinos in
Low-Threshold Dark Matter Detectors
2202.01254 [abs] [pdf]
[abstract]
by Thomas Schwemberger and Tien-Tien Yu.
As low-threshold dark matter detectors advance in development, they will
become sensitive to recoils from solar neutrinos which opens up the possibility
to explore neutrino properties. We predict the enhancement of the event rate of
solar neutrino scattering from Beyond the Standard Model interactions in
low-threshold DM detectors, with a focus on silicon, germanium, gallium
arsenide, xenon, and argon-based detectors. We consider a set of general
neutrino interactions, which fall into five categories: the neutrino magnetic
moment as well as interactions mediated by four types of mediators (scalar,
pseudoscalar, vector, and axial vector), and consider coupling these mediators
to either quarks or electrons. Using these predictions, we place constraints on
the mass and couplings of each mediator and the neutrino magnetic moment from
current low-threshold detectors like SENSEI, Edelweiss, and SuperCDMS, as well
as projections relevant for future experiments such as DAMIC-M, Oscura, Darwin,
and ARGO. We find that such low-threshold detectors can improve current
constraints by up to two orders of magnitude for vector mediators and one order
of magnitude for scalar mediators.
January 2022
Influence of cross-sectional uncertainty on sensitivity studies of DUNE
and T2HK experiments
2201.08040 [abs] [pdf]
[abstract]
by Ritu Devi, Jaydip Singh, and Baba Potukuchi.
The ultimate objectives of ongoing and upcoming neutrino experiments are the
precise measurement of neutrino mixing parameters and the confirmation of mass
hierarchy. The systematic inaccuracy in the cross-section models introduces
inaccuracy in the neutrino mixing parameters estimation. It is important to
secure a large decrease of uncertainties, particularly those relating to
cross-section, neutrino-nucleus interactions, and neutrino-energy
reconstruction, in order to achieve these ambitious goals. In this research
article, we use three alternative neutrino event generators, GENIE, NuWro, and
GiBUU, to analyze sensitivity studies of T2HK, DUNE, and combined sensitivity
of DUNE, and T2HK for mass hierarchy, CP violation, and octant degeneracy
caused by cross-section uncertainties. The cross-section models of these
generators are separate and independent.
Can NSI affect non-local correlations in neutrino oscillations?
2201.05580 [abs] [pdf]
[abstract]
by Bhavna Yadav, [and 3 more]Trisha Sarkar, Khushboo Dixit, and Ashutosh Kumar Alok [hide authors].
Non-local correlations in entangled systems are usually captured by measures
such as Bell's inequality violation. It was recently shown that in neutrino
systems, a measure of non-local advantage of quantum coherence (NAQC) can be
considered as a stronger measure of non-local correlations as compared to the
Bell's inequality violation. In this work, we analyze the effects of non
standard interaction (NSI) on these measures in the context of two flavour
neutrino oscillations for DUNE, MINOS, T2K, KamLAND, JUNO and Daya Bay
experimental set-ups. We find that even in the presence of NSI, Bell's
inequality violation occurs in the entire energy range whereas the NAQC
violation is observed only in some specific energy range justifying the more
elementary feature of NAQC. Further, we find that NSI can enhance the violation
of NAQC and Bell's inequality parameter in the higher energy range of a given
experimental set-up; these enhancements being maximal for the KamLAND
experiment. However, the possible enhancement in the violation of the Bell's
inequality parameter over the standard model prediction can be up to 11%
whereas for NAQC it is 7%. Thus although NAQC is a comparatively stronger
witness of nonclassicality, it shows lesser sensitivity to NSI effects in
comparison to the Bell's inequality parameter.
Impact of Wave Packet Separation in Low-Energy Sterile Neutrino Searches
2201.05108 [abs] [pdf]
[abstract]
by Carlos A. Argüelles, Toni Bertólez-Martínez, and Jordi Salvado.
Light sterile neutrinos have been motivated by anomalies observed in
short-baseline neutrino experiments.Among them, radioactive-source and reactor
experiments have provided evidence and constraints, respectively, for electron
neutrino disappearance compatible with an eV-scale neutrino. The results from
these observations are seemingly in conflict. This letter brings into focus the
assumption that the neutrino wave packet can be approximated as a plane wave,
which is adopted in all analyses of such experiments. We demonstrate that the
damping of oscillations, e.g., due to a finite wave packet size, solve the
tension between these electron-flavor observations and constraints.
Constraining Light Mediators via Detection of Coherent Elastic Solar
Neutrino Nucleus Scattering
2201.05015 [abs] [pdf]
[abstract]
by Yu-Feng Li and Shuo-yu Xia.
Dark matter (DM) direct detection experiments are entering the multiple-ton
era and will be sensitive to the coherent elastic neutrino nucleus scattering
(CE$\nu$NS) of solar neutrinos, enabling the possibility to explore
contributions from new physics with light mediators at the low energy range. In
this paper we consider light mediator models (scalar, vector and axial vector)
and the corresponding contributions to the solar neutrino CE$\nu$NS process.
Motivated by the current status of new generation of DM direct detection
experiments and the future plan, we study the sensitivity of light mediators in
DM direct detection experiments of different nuclear targets and detector
techniques. The constraints from the latest $^8$B solar neutrino measurements
of XENON-1T are also derived. Finally, We show that the solar neutrino
CE$\nu$NS process can provide stringent limitation on the $ L_{\mu}-L_{\tau} $
model with the vector mediator mass below 100 MeV, covering the viable
parameter space of the solution to the $ (g-2)_{\mu}$ anomaly.
Strong constraints on neutrino nonstandard interactions from TeV-scale
$ν_μ$ disappearance at IceCube
2201.03566 [abs] [pdf]
[abstract]
by IceCube Collaboration, [and 383 more]R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, J. M. Alameddine, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Axani, X. Bai, A. Balagopal V., S. W. Barwick, B. Bastian, V. Basu, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. Benda, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, M. Boddenberg, F. Bontempo, J. Borowka, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, F. Bradascio, J. Braun, B. Brinson, S. Bron, J. Brostean-Kaiser, S. Browne, A. Burgman, R. T. Burley, R. S. Busse, M. A. Campana, E. G. Carnie-Bronca, C. Chen, Z. Chen, D. Chirkin, K. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, C. Dappen, P. Dave, C. De Clercq, J. J. DeLaunay, D. Delgado López, H. Dembinski, K. Deoskar, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, H. Dujmovic, M. Dunkman, M. A. DuVernois, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, K. L. Fan, A. R. Fazely, A. Fedynitch, N. Feigl, S. Fiedlschuster, A. T. Fienberg, K. Filimonov, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, A. Garcia, S. Garrappa, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glauch, T. Glüsenkamp, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, S. Griswold, C. Günther, P. Gutjahr, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, M. Ha Minh, K. Hanson, J. Hardin, A. A. Harnisch, A. Haungs, D. Hebecker, K. Helbing, F. Henningsen, E. C. Hettinger, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, K. Hymon, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, M. Jin, B. J. P. Jones, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, L. Kardum, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, K. Kin, T. Kintscher, J. Kiryluk, S. R. Klein, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, T. Kozynets, E. Kun, N. Kurahashi, N. Lad, C. Lagunas Gualda, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, J. W. Lee, K. Leonard, A. Leszczyńska, Y. Li, M. Lincetto, Q. R. Liu, M. Liubarska, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, S. Mancina, I. C. Mari{ş}, I. Martinez-Soler, R. Maruyama, S. McCarthy, T. McElroy, F. McNally, J. V. Mead, K. Meagher, S. Mechbal, A. Medina, M. Meier, S. Meighen-Berger, J. Micallef, D. Mockler, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, R. Naab, R. Nagai, U. Naumann, J. Necker, L. V. Nguy{\~{ê}}n, H. Niederhausen, M. U. Nisa, S. C. Nowicki, A. Obertacke Pollmann, M. Oehler, B. Oeyen, A. Olivas, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, L. Paul, C. Pérez de los Heros, L. Peters, J. Peterson, S. Philippen, S. Pieper, M. Pittermann, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, B. Pries, G. T. Przybylski, C. Raab, J. Rack-Helleis, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, Z. Rechav, A. Rehman, P. Reichherzer, R. Reimann, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, E. J. Roberts, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, J. Saffer, S. E. Sanchez Herrera, A. Sandrock, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Schaufel, H. Schieler, S. Schindler, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, G. Schwefer, S. Sclafani, D. Seckel, S. Seunarine, A. Sharma, S. Shefali, N. Shimizu, M. Silva, B. Skrzypek, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, C. Spannfellner, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, T. Stezelberger, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, S. Ter-Antonyan, J. Thwaites, S. Tilav, F. Tischbein, K. Tollefson, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, C. F. Turley, J. P. Twagirayezu, B. Ty, M. A. Unland Elorrieta, N. Valtonen-Mattila, J. Vandenbroucke, N. van Eijndhoven, D. Vannerom, J. van Santen, J. Veitch-Michaelis, S. Verpoest, C. Walck, W. Wang, T. B. Watson, C. Weaver, P. Weigel, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. H. Wiebusch, D. R. Williams, M. Wolf, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, J. P. Yanez, E. Yildizci, S. Yoshida, S. Yu, T. Yuan, Z. Zhang, and P. Zhelnin [hide authors].
We report a search for nonstandard neutrino interactions (NSI) using eight
years of TeV-scale atmospheric muon neutrino data from the IceCube Neutrino
Observatory. By reconstructing incident energies and zenith angles for
atmospheric neutrino events, this analysis presents unified confidence
intervals for the NSI parameter $\epsilon_{\mu \tau}$. The best-fit value is
consistent with no NSI at a p-value of 25.2%. With a 90% confidence interval of
$-0.0041 \leq \epsilon_{\mu \tau} \leq 0.0031$ along the real axis and similar
strength in the complex plane, this result is the strongest constraint on any
NSI parameter from any oscillation channel to date.
MiniBooNE and MicroBooNE Combined Fit to a 3+1 Sterile Neutrino Scenario
2201.01724 [abs] [pdf]
[abstract]
by A. A. Aguilar-Arevalo, [and 38 more]B. C. Brown, J. M. Conrad, R. Dharmapalan, A. Diaz, Z. Djurcic, D. A. Finley, R. Ford, G. T. Garvey, S. Gollapinni, A. Hourlier, E. -C. Huang, N. W. Kamp, G. Karagiorgi, T. Katori, T. Kobilarcik, K. Lin, W. C. Louis, C. Mariani, W. Marsh, G. B. Mills, J. Mirabal-Martinez, C. D. Moore, R. H. Nelson, J. Nowak, Z. Pavlovic, H. Ray, B. P. Roe, A. D. Russell, A. Schneider, M. H. Shaevitz, J. Spitz, I. Stancu, R. Tayloe, R. T. Thornton, M. Tzanov, R. G. Van de Water, D. H. White, and E. D. Zimmerman [hide authors].
This letter presents the results from the MiniBooNE experiment within a full
"3+1" scenario where one sterile neutrino is introduced to the
three-active-neutrino picture. In addition to electron-neutrino appearance at
short-baselines, this scenario also allows for disappearance of the
muon-neutrino and electron-neutrino fluxes in the Booster Neutrino Beam, which
is shared by the MicroBooNE experiment. We present the 3+1 fit to the MiniBooNE
electron-(anti)neutrino and muon-(anti)neutrino data alone, and in combination
with MicroBooNE electron-neutrino data. The best-fit parameters of the combined
fit with the exclusive CCQE analysis (inclusive analysis) are $\Delta m^2 =
0.29 eV^2 (0.33 eV^2)$, $|U_{e4}|^2 = 0.016 (0.500)$, $|U_{\mu 4}|^2 = 0.500
(0.500)$, and $\sin^2(2\theta_{\mu e})=0.0316 (1.0)$. Comparing the
no-oscillation scenario to the 3+1 model, the data prefer the 3+1 model with a
$\Delta \chi^2/\text{dof} = 24.7 / 3 (17.3 / 3)$, a $4.3\sigma (3.4\sigma)$
preference assuming the asymptotic approximation given by Wilks' theorem.
December 2021
Search for non-standard neutrino interactions with 10 years of ANTARES
data
2112.14517 [abs] [pdf]
[abstract]
by A. Albert, [and 147 more]S. Alves, M. André, M. Anghinolfi, G. Anton, M. Ardid, S. Ardid, J. -J. Aubert, J. Aublin, B. Baret, S. Basa, B. Belhorma, M. Bendahman, F. Benfenati, V. Bertin, S. Biagi, M. Bissinger, J. Boumaaza, M. Bouta, M. C. Bouwhuis, H. Brânzas, R. Bruijn, J. Brunner, J. Busto, B. Caiffi, D. Calvo, A. Capone, L. Caramete, J. Carr, V. Carretero, S. Celli, M. Chabab, T. N. Chau, R. Cherkaoui El Moursli, T. Chiarusi, M. Circella, A. Coleiro, R. Coniglione, P. Coyle, A. Creusot, A. F. Díaz, G. de Wasseige, C. Distefano, I. Di Palma, A. Domi, C. Donzaud, D. Dornic, D. Drouhin, T. Eberl, T. van Eeden, D. van Eijk, N. El Khayati, A. Enzenhöfer, P. Fermani, G. Ferrara, F. Filippini, L. Fusco, Y. Gatelet, P. Gay, H. Glotin, R. Gozzini, R. Gracia Ruiz, K. Graf, C. Guidi, S. Hallmann, H. van Haren, A. J. Heijboer, Y. Hello, J. J. Hernández-Rey, J. Hößl, J. Hofestädt, F. Huang, G. Illuminati, C. W. James, B. Jisse-Jung, M. de Jong, P. de Jong, M. Kadler, O. Kalekin, U. Katz, N. R. Khan-Chowdhury, A. Kouchner, I. Kreykenbohm, V. Kulikovskiy, R. Lahmann, R. Le Breton, S. LeStum, D. Lefèvre, E. Leonora, G. Levi, M. Lincetto, D. Lopez-Coto, S. Loucatos, L. Maderer, J. Manczak, M. Marcelin, A. Margiotta, A. Marinelli, J. A. Martínez-Mora, B. Martino, K. Melis, P. Migliozzi, A. Moussa, R. Muller, L. Nauta, S. Navas, E. Nezri, B. Ó Fearraigh, A. Paun, G. E. Pavalas, C. Pellegrino, M. Perrin-Terrin, V. Pestel, P. Piattelli, C. Pieterse, C. Poirè, V. Popa, T. Pradier, N. Randazzo, D. Real, S. Reck, G. Riccobene, A. Romanov, A. Sánchez-Losa, F. Salesa Greus, D. F. E. Samtleben, M. Sanguineti, P. Sapienza, J. Schnabel, J. Schumann, F. Schüssler, J. Seneca, M. Spurio, Th. Stolarczyk, M. Taiuti, Y. Tayalati, T. Thakore, S. J. Tingay, B. Vallage, V. Van Elewyck, F. Versari, S. Viola, D. Vivolo, J. Wilms, S. Zavatarelli, A. Zegarelli, J. D. Zornoza, and J. Zúñiga [hide authors].
Non-standard interactions of neutrinos arising in many theories beyond the
Standard Model can significantly alter matter effects in atmospheric neutrino
propagation through the Earth. In this paper, a search for deviations from the
prediction of the standard 3-flavour atmospheric neutrino oscillations using
the data taken by the ANTARES neutrino telescope is presented. Ten years of
atmospheric neutrino data collected from 2007 to 2016, with reconstructed
energies in the range from $\sim$16 GeV to $100$ GeV, have been analysed. A
log-likelihood ratio test of the dimensionless coefficients
$\varepsilon_{\mu\tau}$ and $\varepsilon_{\tau\tau} - \varepsilon_{\mu\mu}$
does not provide clear evidence of deviations from standard interactions. For
normal neutrino mass ordering, the combined fit of both coefficients yields a
value 1.7$\sigma$ away from the null result. However, the 68% and 95%
confidence level intervals for $\varepsilon_{\mu\tau}$ and
$\varepsilon_{\tau\tau} - \varepsilon_{\mu\mu}$, respectively, contain the null
value. Best fit values, one standard deviation errors and bounds at the 90%
confidence level for these coefficients are given for both normal and inverted
mass orderings. The constraint on $\varepsilon_{\mu\tau}$ is among the most
stringent to date and it further restrains the strength of possible
non-standard interactions in the $\mu - \tau$ sector.
Damping signatures at JUNO, a medium-baseline reactor neutrino
oscillation experiment
2112.14450 [abs] [pdf]
[abstract]
by JUNO collaboration, [and 606 more]Jun Wang, Jiajun Liao, Wei Wang, Angel Abusleme, Thomas Adam, Shakeel Ahmad, Rizwan Ahmed, Sebastiano Aiello, Muhammad Akram, Fengpeng An, Qi An, Giuseppe Andronico, Nikolay Anfimov, Vito Antonelli, Tatiana Antoshkina, Burin Asavapibhop, João Pedro Athayde Marcondes de André, Didier Auguste, Andrej Babic, Nikita Balashov, Wander Baldini, Andrea Barresi, Davide Basilico, Eric Baussan, Marco Bellato, Antonio Bergnoli, Thilo Birkenfeld, Sylvie Blin, David Blum, Simon Blyth, Anastasia Bolshakova, Mathieu Bongrand, Clément Bordereau, Dominique Breton, Augusto Brigatti, Riccardo Brugnera, Riccardo Bruno, Antonio Budano, Mario Buscemi, Jose Busto, Ilya Butorov, Anatael Cabrera, Hao Cai, Xiao Cai, Yanke Cai, Zhiyan Cai, Riccardo Callegari, Antonio Cammi, Agustin Campeny, Chuanya Cao, Guofu Cao, Jun Cao, Rossella Caruso, Cédric Cerna, Jinfan Chang, Yun Chang, Pingping Chen, Po-An Chen, Shaomin Chen, Xurong Chen, Yi-Wen Chen, Yixue Chen, Yu Chen, Zhang Chen, Jie Cheng, Yaping Cheng, Alexey Chetverikov, Davide Chiesa, Pietro Chimenti, Artem Chukanov, Gérard Claverie, Catia Clementi, Barbara Clerbaux, Selma Conforti Di Lorenzo, Daniele Corti, Flavio Dal Corso, Olivia Dalager, Christophe De La Taille, Jiawei Deng, Zhi Deng, Ziyan Deng, Wilfried Depnering, Marco Diaz, Xuefeng Ding, Yayun Ding, Bayu Dirgantara, Sergey Dmitrievsky, Tadeas Dohnal, Dmitry Dolzhikov, Georgy Donchenko, Jianmeng Dong, Evgeny Doroshkevich, Marcos Dracos, Frédéric Druillole, Ran Du, Shuxian Du, Stefano Dusini, Martin Dvorak, Timo Enqvist, Heike Enzmann, Andrea Fabbri, Lukas Fajt, Donghua Fan, Lei Fan, Jian Fang, Wenxing Fang, Marco Fargetta, Dmitry Fedoseev, Vladko Fekete, Li-Cheng Feng, Qichun Feng, Richard Ford, Amélie Fournier, Haonan Gan, Feng Gao, Alberto Garfagnini, Arsenii Gavrikov, Marco Giammarchi, Agnese Giaz, Nunzio Giudice, Maxim Gonchar, Guanghua Gong, Hui Gong, Yuri Gornushkin, Alexandre Göttel, Marco Grassi, Christian Grewing, Vasily Gromov, Minghao Gu, Xiaofei Gu, Yu Gu, Mengyun Guan, Nunzio Guardone, Maria Gul, Cong Guo, Jingyuan Guo, Wanlei Guo, Xinheng Guo, Yuhang Guo, Paul Hackspacher, Caren Hagner, Ran Han, Yang Han, Muhammad Sohaib Hassan, Miao He, Wei He, Tobias Heinz, Patrick Hellmuth, Yuekun Heng, Rafael Herrera, YuenKeung Hor, Shaojing Hou, Yee Hsiung, Bei-Zhen Hu, Hang Hu, Jianrun Hu, Jun Hu, Shouyang Hu, Tao Hu, Zhuojun Hu, Chunhao Huang, Guihong Huang, Hanxiong Huang, Wenhao Huang, Xin Huang, Xingtao Huang, Yongbo Huang, Jiaqi Hui, Lei Huo, Wenju Huo, Cédric Huss, Safeer Hussain, Ara Ioannisian, Roberto Isocrate, Beatrice Jelmini, Kuo-Lun Jen, Ignacio Jeria, Xiaolu Ji, Xingzhao Ji, Huihui Jia, Junji Jia, Siyu Jian, Di Jiang, Wei Jiang, Xiaoshan Jiang, Ruyi Jin, Xiaoping Jing, Cécile Jollet, Jari Joutsenvaara, Sirichok Jungthawan, Leonidas Kalousis, Philipp Kampmann, Li Kang, Rebin Karaparambil, Narine Kazarian, Khanchai Khosonthongkee, Denis Korablev, Konstantin Kouzakov, Alexey Krasnoperov, Andre Kruth, Nikolay Kutovskiy, Pasi Kuusiniemi, Tobias Lachenmaier, Cecilia Landini, Sébastien Leblanc, Victor Lebrin, Frederic Lefevre, Ruiting Lei, Rupert Leitner, Jason Leung, Demin Li, Fei Li, Fule Li, Haitao Li, Huiling Li, Jiaqi Li, Mengzhao Li, Min Li, Nan Li, Nan Li, Qingjiang Li, Ruhui Li, Shanfeng Li, Tao Li, Weidong Li, Weiguo Li, Xiaomei Li, Xiaonan Li, Xinglong Li, Yi Li, Yufeng Li, Zhaohan Li, Zhibing Li, Ziyuan Li, Hao Liang, Hao Liang, Daniel Liebau, Ayut Limphirat, Sukit Limpijumnong, Guey-Lin Lin, Shengxin Lin, Tao Lin, Jiajie Ling, Ivano Lippi, Fang Liu, Haidong Liu, Hongbang Liu, Hongjuan Liu, Hongtao Liu, Hui Liu, Jianglai Liu, Jinchang Liu, Min Liu, Qian Liu, Qin Liu, Runxuan Liu, Shuangyu Liu, Shubin Liu, Shulin Liu, Xiaowei Liu, Xiwen Liu, Yan Liu, Yunzhe Liu, Alexey Lokhov, Paolo Lombardi, Claudio Lombardo, Kai Loo, Chuan Lu, Haoqi Lu, Jingbin Lu, Junguang Lu, Shuxiang Lu, Xiaoxu Lu, Bayarto Lubsandorzhiev, Sultim Lubsandorzhiev, Livia Ludhova, Arslan Lukanov, Fengjiao Luo, Guang Luo, Pengwei Luo, Shu Luo, Wuming Luo, Vladimir Lyashuk, Bangzheng Ma, Qiumei Ma, Si Ma, Xiaoyan Ma, Xubo Ma, Jihane Maalmi, Yury Malyshkin, Roberto Carlos Mandujano, Fabio Mantovani, Francesco Manzali, Xin Mao, Yajun Mao, Stefano M. Mari, Filippo Marini, Sadia Marium, Cristina Martellini, Gisele Martin-Chassard, Agnese Martini, Matthias Mayer, Davit Mayilyan, Ints Mednieks, Yue Meng, Anselmo Meregaglia, Emanuela Meroni, David Meyhöfer, Mauro Mezzetto, Jonathan Miller, Lino Miramonti, Paolo Montini, Michele Montuschi, Axel Müller, Massimiliano Nastasi, Dmitry V. Naumov, Elena Naumova, Diana Navas-Nicolas, Igor Nemchenok, Minh Thuan Nguyen Thi, Feipeng Ning, Zhe Ning, Hiroshi Nunokawa, Lothar Oberauer, Juan Pedro Ochoa-Ricoux, Alexander Olshevskiy, Domizia Orestano, Fausto Ortica, Rainer Othegraven, Hsiao-Ru Pan, Alessandro Paoloni, Sergio Parmeggiano, Yatian Pei, Nicomede Pelliccia, Anguo Peng, Haiping Peng, Frédéric Perrot, Pierre-Alexandre Petitjean, Fabrizio Petrucci, Oliver Pilarczyk, Luis Felipe Piñeres Rico, Artyom Popov, Pascal Poussot, Wathan Pratumwan, Ezio Previtali, Fazhi Qi, Ming Qi, Sen Qian, Xiaohui Qian, Zhen Qian, Hao Qiao, Zhonghua Qin, Shoukang Qiu, Muhammad Usman Rajput, Gioacchino Ranucci, Neill Raper, Alessandra Re, Henning Rebber, Abdel Rebii, Bin Ren, Jie Ren, Barbara Ricci, Markus Robens, Mathieu Roche, Narongkiat Rodphai, Aldo Romani, Bedřich Roskovec, Christian Roth, Xiangdong Ruan, Xichao Ruan, Saroj Rujirawat, Arseniy Rybnikov, Andrey Sadovsky, Paolo Saggese, Simone Sanfilippo, Anut Sangka, Nuanwan Sanguansak, Utane Sawangwit, Julia Sawatzki, Fatma Sawy, Michaela Schever, Cédric Schwab, Konstantin Schweizer, Alexandr Selyunin, Andrea Serafini, Giulio Settanta, Mariangela Settimo, Zhuang Shao, Vladislav Sharov, Arina Shaydurova, Jingyan Shi, Yanan Shi, Vitaly Shutov, Andrey Sidorenkov, Fedor Šimkovic, Chiara Sirignano, Jaruchit Siripak, Monica Sisti, Maciej Slupecki, Mikhail Smirnov, Oleg Smirnov, Thiago Sogo-Bezerra, Sergey Sokolov, Julanan Songwadhana, Boonrucksar Soonthornthum, Albert Sotnikov, Ondřej Šrámek, Warintorn Sreethawong, Achim Stahl, Luca Stanco, Konstantin Stankevich, Dušan Štefánik, Hans Steiger, Jochen Steinmann, Tobias Sterr, Matthias Raphael Stock, Virginia Strati, Alexander Studenikin, Shifeng Sun, Xilei Sun, Yongjie Sun, Yongzhao Sun, Narumon Suwonjandee, Michal Szelezniak, Jian Tang, Qiang Tang, Quan Tang, Xiao Tang, Alexander Tietzsch, Igor Tkachev, Tomas Tmej, Marco Danilo Claudio Torri, Konstantin Treskov, Andrea Triossi, Giancarlo Troni, Wladyslaw Trzaska, Cristina Tuve, Nikita Ushakov, Johannes van den Boom, Stefan van Waasen, Guillaume Vanroyen, Vadim Vedin, Giuseppe Verde, Maxim Vialkov, Benoit Viaud, Cornelius Moritz Vollbrecht, Cristina Volpe, Vit Vorobel, Dmitriy Voronin, Lucia Votano, Pablo Walker, Caishen Wang, Chung-Hsiang Wang, En Wang, Guoli Wang, Jian Wang, Kunyu Wang, Lu Wang, Meifen Wang, Meng Wang, Meng Wang, Ruiguang Wang, Siguang Wang, Wei Wang, Wenshuai Wang, Xi Wang, Xiangyue Wang, Yangfu Wang, Yaoguang Wang, Yi Wang, Yi Wang, Yifang Wang, Yuanqing Wang, Yuman Wang, Zhe Wang, Zheng Wang, Zhimin Wang, Zongyi Wang, Muhammad Waqas, Apimook Watcharangkool, Lianghong Wei, Wei Wei, Wenlu Wei, Yadong Wei, Kaile Wen, Liangjian Wen, Christopher Wiebusch, Steven Chan-Fai Wong, Bjoern Wonsak, Diru Wu, Qun Wu, Zhi Wu, Michael Wurm, Jacques Wurtz, Christian Wysotzki, Yufei Xi, Dongmei Xia, Xiaochuan Xie, Yuguang Xie, Zhangquan Xie, Zhizhong Xing, Benda Xu, Cheng Xu, Donglian Xu, Fanrong Xu, Hangkun Xu, Jilei Xu, Jing Xu, Meihang Xu, Yin Xu, Yu Xu, Baojun Yan, Taylor Yan, Wenqi Yan, Xiongbo Yan, Yupeng Yan, Anbo Yang, Changgen Yang, Chengfeng Yang, Huan Yang, Jie Yang, Lei Yang, Xiaoyu Yang, Yifan Yang, Yifan Yang, Haifeng Yao, Zafar Yasin, Jiaxuan Ye, Mei Ye, Ziping Ye, Ugur Yegin, Frédéric Yermia, Peihuai Yi, Na Yin, Xiangwei Yin, Zhengyun You, Boxiang Yu, Chiye Yu, Chunxu Yu, Hongzhao Yu, Miao Yu, Xianghui Yu, Zeyuan Yu, Zezhong Yu, Chengzhuo Yuan, Ying Yuan, Zhenxiong Yuan, Ziyi Yuan, Baobiao Yue, Noman Zafar, Andre Zambanini, Vitalii Zavadskyi, Shan Zeng, Tingxuan Zeng, Yuda Zeng, Liang Zhan, Aiqiang Zhang, Feiyang Zhang, Guoqing Zhang, Haiqiong Zhang, Honghao Zhang, Jiawen Zhang, Jie Zhang, Jin Zhang, Jingbo Zhang, Jinnan Zhang, Peng Zhang, Qingmin Zhang, Shiqi Zhang, Shu Zhang, Tao Zhang, Xiaomei Zhang, Xuantong Zhang, Xueyao Zhang, Yan Zhang, Yinhong Zhang, Yiyu Zhang, Yongpeng Zhang, Yuanyuan Zhang, Yumei Zhang, Zhenyu Zhang, Zhijian Zhang, Fengyi Zhao, Jie Zhao, Rong Zhao, Shujun Zhao, Tianchi Zhao, Dongqin Zheng, Hua Zheng, Minshan Zheng, Yangheng Zheng, Weirong Zhong, Jing Zhou, Li Zhou, Nan Zhou, Shun Zhou, Tong Zhou, Xiang Zhou, Jiang Zhu, Kangfu Zhu, Kejun Zhu, Zhihang Zhu, Bo Zhuang, Honglin Zhuang, Liang Zong, and Jiaheng Zou [hide authors].
We study damping signatures at the Jiangmen Underground Neutrino Observatory
(JUNO), a medium-baseline reactor neutrino oscillation experiment. These
damping signatures are motivated by various new physics models, including
quantum decoherence, $\nu_3$ decay, neutrino absorption, and wave packet
decoherence. The phenomenological effects of these models can be characterized
by exponential damping factors at the probability level. We assess how well
JUNO can constrain these damping parameters and how to disentangle these
different damping signatures at JUNO. Compared to current experimental limits,
JUNO can significantly improve the limits on $\tau_3/m_3$ in the $\nu_3$ decay
model, the width of the neutrino wave packet $\sigma_x$, and the intrinsic
relative dispersion of neutrino momentum $\sigma_{\rm rel}$.
Neutrino oscillations in Earth for probing dark matter inside the core
2112.14201 [abs] [pdf]
[abstract]
by Anuj Kumar Upadhyay, [and 3 more]Anil Kumar, Sanjib Kumar Agarwalla, and Amol Dighe [hide authors].
Atmospheric neutrinos offer the possibility of probing dark matter inside the
core of the Earth in a unique way, through Earth matter effects in neutrino
oscillations. For example, if dark matter constitutes 40% of the mass inside
the core, a detector like ICAL at INO with muon charge identification
capability can be sensitive to it at around 2$\sigma$ confidence level with
1000 kt$\cdot$yr exposure. We demonstrate that while the dark matter profile
will be hard to identify, the baryonic matter profile inside the core can be
probed in a manner complementary to the seismic measurements.
Improved cosmological constraints on the neutrino mass and lifetime
2112.13862 [abs] [pdf]
[abstract]
by Guillermo F. Abellán, [and 5 more]Zackaria Chacko, Abhish Dev, Peizhi Du, Vivian Poulin, and Yuhsin Tsai [hide authors].
We present cosmological constraints on the sum of neutrino masses as a
function of the neutrino lifetime, in a framework in which neutrinos decay into
dark radiation after becoming non-relativistic. We find that in this regime the
cosmic microwave background (CMB), baryonic acoustic oscillations (BAO) and
(uncalibrated) luminosity distance to supernovae from the Pantheon catalog
constrain the sum of neutrino masses $\sum m_\nu$ to obey $\sum m_\nu< 0.42$ eV
at (95$\%$ C.L.). While the the bound has improved significantly as compared to
the limits on the same scenario from Planck 2015, it still represents a
significant relaxation of the constraints as compared to the stable neutrino
case. We show that most of the improvement can be traced to the more precise
measurements of low-$\ell$ polarization data in Planck 2018, which leads to
tighter constraints on $\tau_{\rm reio}$ (and thereby on $A_s$), breaking the
degeneracy arising from the effect of (large) neutrino masses on the amplitude
of the CMB power spectrum.
Neutrino magnetic and electric dipole moments: From measurements to
parameter space
2112.12817 [abs] [pdf]
[abstract]
by D. Aristizabal Sierra, [and 3 more]O. G. Miranda, D. K. Papoulias, and G. Sanchez Garcia [hide authors].
Searches for neutrino magnetic moments/transitions in low energy neutrino
scattering experiments are sensitive to effective couplings which are an
intricate function of the Hamiltonian parameters. We study the parameter space
dependence of these couplings in the Majorana (transitions) and Dirac (moments)
cases, as well as the impact of the current most stringent experimental upper
limits on the fundamental parameters. In the Majorana case we find that for
reactor, short-baseline and solar neutrinos, CP violation can be understood as
a measurement of parameter space vectors misalignments. The presence of
nonvanishing CP phases opens a blind spot region where -- regardless of how
large the parameters are -- no signal can be observed in either reactor or
short-baseline experiments. Identification of these regions requires a
combination of different data sets and allows for the determination of those CP
phases. We point out that stringent bounds not necessarily imply suppressed
Hamiltonian couplings, thus allowing for regions where disparate upper limits
can be simultaneously satisfied. In contrast, in the Dirac case stringent
experimental upper limits necessarily translate into tight bounds on the
fundamental couplings. In terms of parameter space vectors, we provide a
straightforward mapping of experimental information into parameter space.
Depletion of atmospheric neutrino fluxes from parton energy loss
2112.10791 [abs] [pdf]
[abstract]
by François Arleo, Greg Jackson, and Stéphane Peigné.
The phenomenon of fully coherent energy loss (FCEL) in the collisions of
protons on light ions affects the physics of cosmic ray air showers. As an
illustration, we address two closely related observables: hadron production in
forthcoming proton-oxygen collisions at the LHC, and the atmospheric neutrino
fluxes induced by the semileptonic decays of hadrons produced in proton-air
collisions. In both cases, a significant nuclear suppression due to FCEL is
predicted. The conventional and prompt neutrino fluxes are suppressed by $\sim
10...25\%$ in their relevant neutrino energy ranges. Previous estimates of
atmospheric neutrino fluxes should be scaled down accordingly to account for
FCEL.
The Return of the Templates: Revisiting the Galactic Center Excess with
Multi-Messenger Observations
2112.09706 [abs] [pdf]
[abstract]
by Ilias Cholis, [and 3 more]Yi-Ming Zhong, Samuel D. McDermott, and Joseph P. Surdutovich [hide authors].
The Galactic center excess (GCE) remains one of the most intriguing
discoveries from the Fermi Large Area Telescope (LAT) observations. We revisit
the characteristics of the GCE by first producing a new set of high-resolution
galactic diffuse gamma-ray emission templates, which are ultimately due to
cosmic-ray interactions with the interstellar medium. Using multi-messenger
observations we constrain the properties of the galactic diffuse emission. The
broad properties of the GCE that we find in this work are qualitatively
unchanged despite the introduction of this new set of templates, though its
quantitative features appear mildly different than those obtained in previous
analyses. In particular, we find a high-energy tail at higher significance than
previously reported. This tail is very prominent in the northern hemisphere,
and less so in the southern hemisphere. This strongly affects one prominent
interpretation of the excess: known millisecond pulsars are incapable of
producing this high-energy emission, even in the relatively softer southern
hemisphere, and are therefore disfavored as the sole explanation of the GCE.
The annihilation of dark matter particles of mass $40^{+10}_{-7}$ GeV (95$\%$
CL) to $b$ quarks with a cross-section of $\sigma v = 1.4^{+0.6}_{-0.3} \times
10^{-26}$ cm$^{3}$s$^{-1}$ provides a good fit to the excess especially in the
relatively cleaner southern sky. Dark matter of the same mass range
annihilating to $b$ quarks or heavier dark matter particles annihilating to
heavier Standard Model bosons can combine with millisecond pulsars to provide a
good fit to the southern hemisphere emission. As part of this paper, we make
publicly available all of our templates and the data covariance matrix we have
generated to account for systematic uncertainties.[abridged]
Probing New Physics at Future Tau Neutrino Telescopes
2112.09476 [abs] [pdf]
[abstract]
by Guo-yuan Huang, [and 3 more]Sudip Jana, Manfred Lindner, and Werner Rodejohann [hide authors].
We systematically investigate new physics scenarios that can modify the
interactions between neutrinos and matter at upcoming tau neutrino telescopes,
which will test neutrino-proton collisions with energies $ \gtrsim 45~{\rm
TeV}$, and can provide unique insights to the elusive tau neutrino. At such
high energy scales, the impact of parton distribution functions of second and
third generations of quarks (usually suppressed) can be comparable to the
contribution of first generation with small momentum fraction, hence making tau
neutrino telescopes an excellent facility to probe new physics associated with
second and third families. Among an inclusive set of particle physics models,
we identify new physics scenarios at tree level that can give competitive
contributions to the neutrino cross sections while staying within laboratory
constraints: charged/neutral Higgs and leptoquarks. Our analysis is close to
the actual experimental configurations of the telescopes, and we perform a
$\chi^2$-analysis on the energy and angular distributions of the tau events. By
numerically solving the propagation equations of neutrino and tau fluxes in
matter, we obtain the sensitivities of representative upcoming tau neutrino
telescopes, GRAND, POEMMA and Trinity, to the charged Higgs and leptoquark
models. While each of the experiments can achieve a sensitivity better than the
current collider reaches for certain models, their combination is remarkably
complementary in probing the new physics. In particular, the new physics will
affect the energy and angular distributions in different ways at those
telescopes.
Towards Probing the Diffuse Supernova Neutrino Background in All Flavors
2112.09168 [abs] [pdf]
[abstract]
by Anna M. Suliga, John F. Beacom, and Irene Tamborra.
Fully understanding the average core-collapse supernova requires detecting
the diffuse supernova neutrino background (DSNB) in all flavors. While the DSNB
$\bar{\nu}_e$ flux is near detection, and the DSNB $\nu_e$ flux has a good
upper limit and prospects for improvement, the DSNB $\nu_x$ (each of $\nu_\mu,
\nu_\tau, \bar{\nu}_\mu, \bar{\nu}_\tau$) flux has a poor limit and heretofore
had no clear path for improved sensitivity. We show that a succession of
xenon-based dark matter detectors -- XENON1T (completed), XENONnT/LUX-ZEPLIN
(running), and DARWIN (proposed) -- can dramatically improve sensitivity to
DSNB $\nu_x$ the neutrino-nucleus coherent scattering channel. XENON1T could
match the present sensitivity of $\sim 10^3 \;
\mathrm{cm}^{-2}~\mathrm{s}^{-1}$ per $\nu_x$ flavor, XENONnT/LUX-ZEPLIN would
have linear improvement of sensitivity with exposure, and a long run of DARWIN
could reach a flux sensitivity of $\sim 10 \;
\mathrm{cm}^{-2}~\mathrm{s}^{-1}$. Together, these would also contribute to
greatly improve bounds on non-standard scenarios. Ultimately, to reach the
standard flux range of $\sim 1 \; \mathrm{cm}^{-2}~\mathrm{s}^{-1}$, even
larger exposures will be needed, which we show may be possible with the series
of proposed lead-based RES-NOVA detectors.
On T violation in non-standard neutrino oscillation scenarios
2112.08801 [abs] [pdf]
[abstract]
by Thomas Schwetz and Alejandro Segarra.
We discuss time reversal (T) violation in neutrino oscillations in generic
new physics scenarios. A general parameterization is adopted to describe
flavour evolution, which captures a wide range of new physics effects,
including non-standard neutrino interactions, non-unitarity, and sterile
neutrinos in a model-independent way. In this framework, we discuss general
properties of time reversal in the context of long-baseline neutrino
experiments. Special attention is given to fundamental versus environmental T
violation in the presence of generic new physics. We point out that T violation
in the disappearance channel requires new physics which modifies flavour mixing
at neutrino production and detection. We use time-dependent perturbation theory
to study the effect of non-constant matter density along the neutrino path, and
quantify the effects for the well studied baselines of the DUNE, T2HK, and
T2HKK projects. The material presented here provides the phenomenological
background for the model-independent test of T violation proposed by us in Ref.
[1].
Excess of Tau events at SND@LHC, FASER$ν$ and FASER$ν$2
2112.08799 [abs] [pdf]
[abstract]
by Saeed Ansarifard and Yasaman Farzan.
During the run III of the LHC, the forward experiments FASER$\nu$ and SND@LHC
will be able to detect the Charged Current (CC) interactions of the high energy
neutrinos of all three flavors produced at the ATLAS Interaction Point (IP).
This opportunity may unravel mysteries of the third generation leptons. We
build three models that can lead to a tau excess at these detectors through the
following Lepton Flavor Violating (LFV) beyond Standard Model (SM) processes:
(1) $\pi^+ \to \mu^+ \nu_\tau$; (2) $\pi^+ \to \mu^+ \bar{\nu}_\tau$ and (3)
$\nu_e+{\rm nucleus}\to \tau +X$. We comment on the possibility of solving the
$(g-2)_\mu$ anomaly and the $\tau$ decay anomalies within these models. We
study the potential of the forward experiments to discover the $\tau$ excess or
to constrain these models in case of no excess. We then compare the reach of
the forward experiments with that of the previous as well as next generation
experiments such as DUNE. We also discuss how the upgrade of FASER$\nu$ can
distinguish between these models by studying the energy spectrum of the tau.
Tau Appearance from High-Energy Neutrino Interactions
2112.06937 [abs] [pdf]
[abstract]
by Alfonso Garcia Soto, [and 3 more]Pavel Zhelnin, Ibrahim Safa, and Carlos A. Argüelles [hide authors].
High-energy muon- and electron-neutrinos yield a non-negligible flux of tau
neutrinos as they propagate through Earth. In this letter, we address the
impact of this additional component in the PeV and EeV energy regimes for the
first time. This contribution is predicted to be significantly larger than the
atmospheric background above 300 TeV, and alters current and future neutrino
telescopes' capabilities to discover a cosmic tau-neutrino flux. Further we
demonstrate that Earthskimming neutrino experiments, designed to observe tau
neutrinos, will be sensitive to cosmogenic neutrinos even in extreme scenarios
without a primary tau-neutrino component.
Toward diagnosing neutrino non-unitarity through CP phase correlations
2112.06178 [abs] [pdf]
[abstract]
by Hisakazu Minakata.
We discuss correlations between the $\nu$SM CP phase $\delta$ and the phases
that originate from new physics which causes neutrino-sector unitarity
violation (UV) at low energies. This study is motivated to provide one of the
building pieces for a machinery to diagnose non-unitarity, our ultimate goal.
We extend the perturbation theory of neutrino oscillation in matter proposed by
Denton {\it et al.}~(DMP) to include the UV effect expressed by the $\alpha$
parametrization. By analyzing the DMP-UV perturbation theory to first order, we
are able to draw a completed picture of the $\delta$ - UV phase correlations in
the whole kinematical region covered by the terrestrial neutrino experiments.
There exist the two regions with the characteristically different patterns of
the correlations: (1) the chiral-type $[e^{- i \delta } \alpha_{\mu e}, ~e^{ -
i \delta} \alpha_{\tau e}, ~\alpha_{\tau \mu}]$ (PDG convention) correlation in
the entire high-energy region $\vert \rho E \vert \gsim 6~(\text{g/cm}^3)$ GeV,
and (2) (blobs of the $\alpha$ parameters) - $e^{ \pm i \delta}$ correlation in
anywhere else. Some relevant aspects for measurement of the UV parameters, such
as the necessity of determining all the $\alpha_{\beta \gamma}$ elements at
once, are also pointed out.
Neutrino Transition in Dark Matter
2112.05057 [abs] [pdf]
[abstract]
by Eung Jin Chun.
An ultralight dark matter may have interesting implications in neutrino
physics which have been studied actively in recent years. It is pointed out
that there appears yet unexplored medium effect in neutrino transitions which
occurs at the first order in perturbation of the neutrino-medium interaction.
We derive the general formula for the neutrino transition probability in a
medium which describes the standard neutrino oscillation as well as the new
medium contribution. It turns out that such an effect constrains the model
parameter space more than ever.
Neutrino Mass Bounds in the era of Tension Cosmology
2112.02993 [abs] [pdf]
[abstract]
by Eleonora Di Valentino and Alessandro Melchiorri.
The measurements of Cosmic Microwave Background anisotropies made by the
Planck satellite provide extremely tight upper bounds on the total neutrino
mass scale ($\Sigma m_{\nu}<0.26 eV$ at $95\%$ C.L.). However, as recently
discussed in the literature, Planck data show anomalies that could affect this
result. Here we provide new constraints on neutrino masses using the recent and
complementary CMB measurements from the Atacama Cosmology Telescope DR4 and the
South Polar Telescope SPT-3G experiments. We found that both the ACT-DR4 and
SPT-3G data, when combined with WMAP, mildly suggest a neutrino mass with
$\Sigma m_{\nu}=0.68 \pm 0.31$ eV and $\Sigma m_{\nu}=0.46_{-0.36}^{+0.14}$ eV
at $68 \%$ C.L, respectively. Moreover, when CMB lensing from the Planck
experiment is included, the ACT-DR4 data now indicates a neutrino mass above
the two standard deviations, with $\Sigma m_{\nu}=0.60_{-0.50}^{+0.44}$ eV at
$95 \%$, while WMAP+SPT-3G provides a weak upper limit of $\Sigma m_{\nu}<0.37$
eV at $68 \%$ C.L.. Interestingly, these results are consistent with the Planck
CMB+Lensing constraint of $\Sigma m_{\nu} = 0.41_{-0.25}^{+0.17}$ eV at $68 \%$
C.L. when variation in the $A_{\rm lens}$ parameter are considered. We also
show that these indications are still present after the inclusion of BAO or
SN-Ia data in extended cosmologies that are usually considered to solve the
so-called Hubble tension. A combination of ACT-DR4, WMAP, BAO and constraints
on the Hubble constant from the SH0ES collaboration gives $\Sigma
m_{\nu}=0.39^{+0.13}_{-0.25}$ eV at $68 \%$ C.L. in extended cosmologies. We
conclude that a total neutrino mass above the $0.26$ eV limit still provides an
excellent fit to several cosmological data and that future data must be
considered before safely ruling it out.
Time- and space-varying neutrino masses from soft topological defects
2112.02107 [abs] [pdf]
[abstract]
by Gia Dvali, Lena Funcke, and Tanmay Vachaspati.
We study the formation and evolution of topological defects that arise in the
post-recombination phase transition predicted by the gravitational neutrino
mass model in [Dvali, Funcke, 2016]. In the transition, global skyrmions,
monopoles, strings, and domain walls form due to the spontaneous breaking of
the neutrino flavor symmetry. These defects are unique in their softness and
origin, as they appear at a very low energy scale, they only require Standard
Model particle content, and they differ fundamentally depending on the Majorana
or Dirac nature of the neutrinos. One of the observational signatures is the
time- and space-dependence of the neutrino mass matrix, which could be
observable in future experiments such as DUNE or in the event of a near-future
galactic supernova explosion. Already existing data rules out parts of the
parameter space in the Majorana case. The detection of this effect could shed
light onto the open question of the Dirac versus Majorana neutrino nature.
Short-baseline oscillation scenarios at JUNO and TAO
2112.00379 [abs] [pdf]
[abstract]
by V. S. Basto-Gonzalez, [and 4 more]D. V. Forero, C. Giunti, A. A. Quiroga, and C. A. Ternes [hide authors].
We study the sensitivity of JUNO and TAO to the oscillations induced by two
well-motivated scenarios beyond the standard model: Large Extra Dimensions
(LED) and light sterile neutrinos in the context of 3+1 neutrino mixing. We
find that JUNO+TAO can set competitive bounds on the parameter space of each
scenario. In particular, we find that JUNO+TAO can be competitive with MINOS,
DUNE or KATRIN in the context of LED. If LED are present in nature, we show
that the parameters could be measured with a similar precision as the standard
oscillation parameters. We also show that JUNO+TAO can test nearly all of the
parameter space preferred by Gallium experiments in the context of 3+1 mixing.
Finally, we discuss the possibility to distinguish the two scenarios from each
other.
November 2021
Leptogenesis and eV scale sterile neutrino
2111.14719 [abs] [pdf]
[abstract]
by Srubabati Goswami, [and 3 more]Vishnudath K. N., Ananya Mukherjee, and Nimmala Narendra [hide authors].
We consider the minimal extended seesaw model which can accommodate an eV
scale sterile neutrino. The scenario also includes three heavy right handed
neutrinos in addition to the light sterile neutrino. In this model, the
active-sterile mixing act as non-unitary parameters. If the values of these
mixing angles are of $\mathcal{O}(0.1)$, the model introduces deviation of the
PMNS matrix from unitarity to this order. We find that the oscillation data
from various experiments imposes an upper bound on the lightest heavy neutrino
mass scale as $\sim 10^{11}$ GeV in the context of this model. We study {\it
vanilla} leptogenesis in this scheme, where the decay of the heavy right handed
neutrinos in the early universe can give rise to the observed baryon asymmetry.
Here, even though the eV scale sterile neutrino does not participate directly
in leptogenesis, its effect is manifested through the non-unitary effects. We
find that the parameter space that can give rise to successful leptogenesis is
constrained by the bounds on the active-sterile mixing as obtained from the
global analysis.
The UHECR dipole and quadrupole in the latest data from the original
Auger and TA surface detectors
2111.14593 [abs] [pdf]
[abstract]
by Peter Tinyakov, [and 15 more]Luis Anchordoqui, Teresa Bister, Jonathan Biteau, Lorenzo Caccianiga, Rogério de Almeida, Olivier Deligny, Armando di Matteo, Ugo Giaccari, Diego Harari, Jihyun Kim, Mikhail Kuznetsov, Ioana Mariş, Grigory Rubtsov, Sergey Troitsky, and Federico Urban [hide authors].
The sources of ultra-high-energy cosmic rays are still unknown, but assuming
standard physics, they are expected to lie within a few hundred megaparsecs
from us. Indeed, over cosmological distances cosmic rays lose energy to
interactions with background photons, at a rate depending on their mass number
and energy and properties of photonuclear interactions and photon backgrounds.
The universe is not homogeneous at such scales, hence the distribution of the
arrival directions of cosmic rays is expected to reflect the inhomogeneities in
the distribution of galaxies; the shorter the energy loss lengths, the stronger
the expected anisotropies. Galactic and intergalactic magnetic fields can blur
and distort the picture, but the magnitudes of the largest-scale anisotropies,
namely the dipole and quadrupole moments, are the most robust to their effects.
Measuring them with no bias regardless of any higher-order multipoles is not
possible except with full-sky coverage. In this work, we achieve this in three
energy ranges (approximately 8--16 EeV, 16--32 EeV, and 32--$\infty$ EeV) by
combining surface-detector data collected at the Pierre Auger Observatory until
2020 and at the Telescope Array (TA) until 2019, before the completion of the
upgrades of the arrays with new scintillator detectors. We find that the
full-sky coverage achieved by combining Auger and TA data reduces the
uncertainties on the north-south components of the dipole and quadrupole in
half compared to Auger-only results.
Non-minimal Lorentz invariance violation in light of muon anomalous
magnetic moment and long-baseline neutrino oscillation data
2111.14336 [abs] [pdf]
[abstract]
by Hai-Xing Lin, [and 3 more]Pedro Pasquini, Jian Tang, and Sampsa Vihonen [hide authors].
In light of the increasing hints of new physics at the muon $g-2$ and
neutrino oscillation experiments, we consider the recently observed tension in
the long-baseline neutrino oscillation experiments as a potential indication of
Lorentz invariance violation. For this purpose, the latest data from T2K and
NO$\nu$A is analysed in presence of non-minimal Lorentz invariance violation.
Indeed, we find that isotropic violation in dimensions $D =$ 4, 5 and 6 can
alleviate the tension in neutrino oscillation data by 0.4$-$2.4$\sigma$ CL
significance, with the isotropic coefficient $\gamma^{(5)}_{\tau \tau} =$
3.58$\times$10$^{-32}$GeV$^{-1}$ yielding the best fit. At the same time, the
anomalous muon $g-2$ result can be reproduced with an additional non-isotropic
violation of $d^{zt} =$ -1.7$\times$10$^{-25}$. The analysis highlights the
possibility of simultaneous relaxation of experimental tensions with Lorentz
invariance violation of mixed nature.
Neutrino propagation when mass eigenstates and decay eigenstates
mismatch
2111.13128 [abs] [pdf]
[abstract]
by Dibya S. Chattopadhyay, [and 4 more]Kaustav Chakraborty, Amol Dighe, Srubabati Goswami, and S. M. Lakshmi [hide authors].
We point out that the Hermitian and anti-Hermitian components of the
effective Hamiltonian for decaying neutrinos cannot be simultaneously
diagonalized by unitary transformations for all matter densities. We develop a
formalism for the two-flavor neutrino propagation through matter of uniform
density, for neutrino decay to invisible states. Employing a resummation of the
Zassenhaus expansion, we obtain compact analytic expressions for neutrino
survival and conversion probabilities, to first and second order in the
"mismatch parameter" $\bar{\gamma}$.
T-violating effect in $ν_τ (\barν_τ)-$nucleon
quasielastic scattering
2111.13021 [abs] [pdf]
[abstract]
by A. Fatima, M. Sajjad Athar, and S. K. Singh.
The production cross sections and polarization observables of the $\tau$
leptons produced in the $|\Delta S| = 0$ and $1$ induced
$\nu_{\tau}(\bar{\nu}_{\tau})-N$ quasielastic scattering have been studied. The
effect of T violation, in the case of $\Delta S=0$ and 1 processes, and the
SU(3) symmetry breaking effects, in the case of $\Delta S=1$ processes, on the
total scattering cross sections as well polarization observables are explored.
Experimentally, it would be possible to observe these effects in the
forthcoming (anti)neutrino experiments like DUNE, SHiP and DsTau.
Exploring the effects of Scalar Non Standard Interactions on the CP
violation sensitivity at DUNE
2111.12943 [abs] [pdf]
[abstract]
by Abinash Medhi, Debajyoti Dutta, and Moon Moon Devi.
The Neutrino oscillations have provided an excellent opportunity to study
new-physics beyond the Standard Model, popularly known as BSM. The unknown
couplings involving neutrinos, termed non-standard interactions (NSI), may
appear as `new-physics' in different neutrino experiments. The neutrino NSI
offers significant effects on neutrino oscillations and CP-sensitivity, which
may be probed in various neutrino experiments. The idea of neutrinos coupling
with a scalar has evolved recently and looks promising. The effects of scalar
NSI may appear as a perturbation to the neutrino mass matrix in the neutrino
Hamiltonian. It modifies the neutrino mass matrix and may provide a direct
possibility of probing neutrino mass models. As the scalar NSI affects the
neutrino mass matrix in the Hamiltonian, its effect is energy independent.
Moreover, the matter effects due to scalar NSI scales linearly with the matter
density.
In this work, we have performed a model-independent study of the effects of
scalar NSI at long baseline neutrino experiments, taking DUNE as a case study.
We have performed such a thorough study for DUNE for the first time. Various
neutrino parameters may get affected due to the inclusion of scalar NSI as it
modifies the effective mass matrix of neutrinos. We have explored the impact of
scalar NSI in neutrino oscillations and its impact on the measurements of
various mixing parameters. We have probed the effects of scalar NSI on
different oscillation channels relevant to the experiment. We have also
explored the impact of various possible elements in the scalar NSI term on the
CP-violation sensitivity at DUNE.
What can CMB observations tell us about the neutrino distribution
function?
2111.12726 [abs] [pdf]
[abstract]
by James Alvey, Miguel Escudero, and Nashwan Sabti.
Cosmic Microwave Background (CMB) observations have been used extensively to
constrain key properties of neutrinos, such as their mass. However, these
inferences are typically dependent on assumptions about the cosmological model,
and in particular upon the distribution function of neutrinos in the early
Universe. In this paper, we aim to assess the full extent to which CMB
experiments are sensitive to the shape of the neutrino distribution. We
demonstrate that Planck and CMB-S4-like experiments have no prospects for
detecting particular features in the distribution function. Consequently, we
take a general approach and marginalise completely over the form of the
neutrino distribution to derive constraints on the relativistic and
non-relativistic neutrino energy densities, characterised by $N_\mathrm{eff} =
3.0 \pm 0.4$ and $\rho_{\nu,0}^{\rm NR} < 14 \, \mathrm{eV}\,\mathrm{cm}^{-3}$
at 95% CL, respectively. The fact that these are the only neutrino properties
that CMB data can constrain has important implications for neutrino mass limits
from cosmology. Specifically, in contrast to the $\Lambda$CDM case where CMB
and BAO data tightly constrain the sum of neutrinos masses to be $\sum m_\nu <
0.12 \, \mathrm{eV}$, we explicitly show that neutrino masses as large as $\sum
m_\nu \sim 3 \, \mathrm{eV}$ are perfectly consistent with this data.
Importantly, for this to be the case, the neutrino number density should be
suitably small such that the bound on $\rho_{\nu,0}^\mathrm{NR} = \sum m_\nu
n_{\nu,0}$ is still satisfied. We conclude by giving an outlook on the
opportunities that may arise from other complementary experimental probes, such
as galaxy surveys, neutrino mass experiments and facilities designed to
directly detect the cosmic neutrino background.
Statistical significance of the sterile-neutrino hypothesis in the
context of reactor and gallium data
2111.12530 [abs] [pdf]
[abstract]
by Jeffrey M. Berryman, [and 4 more]Pilar Coloma, Patrick Huber, Thomas Schwetz, and Albert Zhou [hide authors].
We evaluate the statistical significance of the 3+1 sterile-neutrino
hypothesis using $\nu_e$ and $\bar\nu_e$ disappearance data from reactor, solar
and gallium radioactive source experiments. Concerning the latter, we
investigate the implications of the recent BEST results. For reactor data we
focus on relative measurements independent of flux predictions. For the problem
at hand, the usual $\chi^2$-approximation to hypothesis testing based on Wilks'
theorem has been shown in the literature to be inaccurate. We therefore present
results based on Monte Carlo simulations, and find that this typically reduces
the significance by roughly $1\,\sigma$ with respect to the na\"ive
expectation. We find no significant indication in favor of sterile-neutrino
oscillations from reactor data. On the other hand, gallium data (dominated by
the BEST result) show more than $5\,\sigma$ of evidence supporting the
sterile-neutrino hypothesis, favoring oscillation parameters in agreement with
constraints from reactor data. This explanation is, however, in significant
tension ($\sim 3\,\sigma$) with solar neutrino experiments. In order to assess
the robustness of the signal for gallium experiments we present a discussion of
the impact of cross-section uncertainties on the results.
A close look on 2-3 mixing angle with DUNE in light of current neutrino
oscillation data
2111.11748 [abs] [pdf]
[abstract]
by Sanjib Kumar Agarwalla, [and 3 more]Ritam Kundu, Suprabh Prakash, and Masoom Singh [hide authors].
Recent global fit analyses of oscillation data show a preference for normal
mass ordering (NMO) at 2.5$\sigma$ and provide 1.6$\sigma$ indications for
lower $\theta_{23}$ octant and leptonic CP violation. A high-precision
measurement of $\theta_{23}$ is pivotal to convert these hints into
discoveries. In this work, we study in detail the capabilities of DUNE to
establish the deviation from maximal $\theta_{23}$ and to resolve its octant at
high confidence levels. We exhibit the possible correlations and degeneracies
among $\sin^2\theta_{23}$, $\Delta m^2_{31}$, and $\delta_{CP}$ in
disappearance and appearance oscillation channels at the probability and event
levels. Introducing for the first time, a bi-events plot in the plane of total
$\nu$ and $\bar\nu$ disappearance events, we discuss the impact of
$\sin^2\theta_{23}$ - $\Delta m^2_{31}$ degeneracy in establishing non-maximal
$\theta_{23}$ and show how this degeneracy can be resolved by exploiting the
spectral shape information in $\nu$ and $\bar\nu$ disappearance events. A
3$\sigma$ (5$\sigma$) determination of non-maximal $\theta_{23}$ is possible in
DUNE in total 7 years if $\sin^2\theta_{23} \lesssim 0.465~(0.450)$ or
$\sin^2\theta_{23} \gtrsim 0.554~(0.572)$ for any value of $\delta_{CP}$ and
NMO. We study the individual contributions from appearance and disappearance
channels, impact of systematic uncertainties and marginalization over
oscillation parameters, importance of spectral analysis and data from both
$\nu$ and $\bar\nu$ runs, while analyzing DUNE's sensitivity to establish
non-maximal $\theta_{23}$. DUNE can resolve the octant of $\theta_{23}$ at
4.2$\sigma$ (5$\sigma$) using 7 (10) years of run assuming $\sin^2\theta_{23}$
= 0.455, $\delta_{CP}$ = $223^\circ$, and NMO. DUNE can improve the current
relative 1$\sigma$ precision on $\sin^2\theta_{23}$ ($\Delta m^2_{31}$) by a
factor of 4.4 (2.8) using 7 years of run.
Improved Characterization of the Astrophysical Muon-Neutrino Flux with
9.5 Years of IceCube Data
2111.10299 [abs] [pdf]
[abstract]
by R. Abbasi, [and 379 more]M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, J. M. Alameddine, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, V. Basu, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, M. Boddenberg, F. Bontempo, J. Borowka, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, F. Bradascio, J. Braun, B. Brinson, S. Bron, J. Brostean-Kaiser, S. Browne, A. Burgman, R. T. Burley, R. S. Busse, M. A. Campana, E. G. Carnie-Bronca, C. Chen, Z. Chen, D. Chirkin, K. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, C. Dappen, P. Dave, C. De Clercq, J. J. DeLaunay, D. Delgado López, H. Dembinski, K. Deoskar, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, H. Dujmovic, M. Dunkman, M. A. DuVernois, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, K. L. Fan, A. R. Fazely, A. Fedynitch, N. Feigl, S. Fiedlschuster, A. T. Fienberg, K. Filimonov, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, A. Garcia, S. Garrappa, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glauch, T. Glüsenkamp, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, S. Griswold, C. Günther, P. Gutjahr, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, M. Ha Minh, K. Hanson, J. Hardin, A. A. Harnisch, A. Haungs, D. Hebecker, K. Helbing, F. Henningsen, E. C. Hettinger, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, K. Hymon, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, M. Jin, B. J. P. Jones, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, L. Kardum, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, K. Kin, T. Kintscher, J. Kiryluk, S. R. Klein, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, T. Kozynets, E. Kun, N. Kurahashi, N. Lad, C. Lagunas Gualda, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, J. W. Lee, K. Leonard, A. Leszczyńska, Y. Li, M. Lincetto, Q. R. Liu, M. Liubarska, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, S. Mancina, I. C. Mariş, I. Martinez-Soler, R. Maruyama, K. Mase, T. McElroy, F. McNally, J. V. Mead, K. Meagher, S. Mechbal, A. Medina, M. Meier, S. Meighen-Berger, J. Micallef, D. Mockler, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, R. Naab, R. Nagai, U. Naumann, J. Necker, L. V. Nguyên, H. Niederhausen, M. U. Nisa, S. C. Nowicki, A. Obertacke Pollmann, M. Oehler, B. Oeyen, A. Olivas, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, L. Paul, C. Pérez de los Heros, L. Peters, J. Peterson, S. Philippen, S. Pieper, M. Pittermann, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, P. B. Price, B. Pries, G. T. Przybylski, C. Raab, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, A. Rehman, P. Reichherzer, R. Reimann, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, E. J. Roberts, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, J. Saffer, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Schaufel, H. Schieler, S. Schindler, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, G. Schwefer, S. Sclafani, D. Seckel, S. Seunarine, A. Sharma, S. Shefali, M. Silva, B. Skrzypek, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, C. Spannfellner, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, S. Ter-Antonyan, S. Tilav, F. Tischbein, K. Tollefson, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, C. F. Turley, J. P. Twagirayezu, B. Ty, M. A. Unland Elorrieta, N. Valtonen-Mattila, J. Vandenbroucke, N. van Eijndhoven, D. Vannerom, J. van Santen, S. Verpoest, C. Walck, T. B. Watson, C. Weaver, P. Weigel, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. H. Wiebusch, D. R. Williams, M. Wolf, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, J. P. Yanez, S. Yoshida, S. Yu, T. Yuan, Z. Zhang, and P. Zhelnin [hide authors].
We present a measurement of the high-energy astrophysical muon-neutrino flux
with the IceCube Neutrino Observatory. The measurement uses a high-purity
selection of ~650k neutrino-induced muon tracks from the Northern celestial
hemisphere, corresponding to 9.5 years of experimental data. With respect to
previous publications, the measurement is improved by the increased size of the
event sample and the extended model testing beyond simple power-law hypotheses.
An updated treatment of systematic uncertainties and atmospheric background
fluxes has been implemented based on recent models. The best-fit single
power-law parameterization for the astrophysical energy spectrum results in a
normalization of $\phi_{\mathrm{@100TeV}}^{\nu_\mu+\bar{\nu}_\mu} =
1.44_{-0.26}^{+0.25} \times
10^{-18}\,\mathrm{GeV}^{-1}\mathrm{cm}^{-2}\mathrm{s}^{-1}\mathrm{sr}^{-1}$ and
a spectral index $\gamma_{\mathrm{SPL}} = 2.37_{-0.09}^{+0.09}$, constrained in
the energy range from $15\,\mathrm{TeV}$ to $5\,\mathrm{PeV}$. The model tests
include a single power law with a spectral cutoff at high energies, a
log-parabola model, several source-class specific flux predictions from the
literature and a model-independent spectral unfolding. The data is well
consistent with a single power law hypothesis, however, spectra with softening
above one PeV are statistically more favorable at a two sigma level.
Neutrino meets ultralight dark matter: $\boldsymbol{0νββ}$
decay and cosmology
2111.08732 [abs] [pdf]
[abstract]
by Guo-yuan Huang and Newton Nath.
We explore the neutrinoless double beta ($0\nu \beta\beta$) decay induced by
an ultralight dark matter field coupled to neutrinos. The effect on
$0\nu\beta\beta$ decay is significant if the coupling violates the lepton
number, for which the $\Delta L=2$ transition is directly driven by the dark
matter field without further suppression of small neutrino masses. As the
ultralight dark matter can be well described by a classical field, the effect
features a periodic modulation pattern in decay events. However, we find that
in the early Universe such coupling will be very likely to alter the standard
cosmological results. In particular, the requirement of neutrino free-streaming
before the matter-radiation equality severely constrains the parameter space,
such that the future $0\nu \beta\beta$ decay experiments can hardly see any
signal even with a meV sensitivity to the effective neutrino mass.
Nonunitarity of the lepton mixing matrix at the European Spallation
Source
2111.08673 [abs] [pdf]
[abstract]
by Sabya Sachi Chatterjee, [and 3 more]O. G. Miranda, M. Tórtola, and J. W. F. Valle [hide authors].
If neutrinos get mass through the exchange of lepton mediators, as in seesaw
schemes, the neutrino appearance probabilities in oscillation experiments are
modified due to effective nonunitarity of the lepton mixing matrix. This also
leads to new CP phases and an ambiguity in underpinning the ''conventional''
phase of the three-neutrino paradigm. We study the CP sensitivities of various
setups based at the European spallation source neutrino super-beam (ESSnuSB)
experiment in the presence of nonunitarity. We also examine its potential in
constraining the associated new physics parameters. Moreover, we show how the
combination of DUNE and ESSnuSB can help further improve the sensitivities on
the nonunitarity parameters.
Non-standard Neutrino and $Z'$ Interactions at the FASER$ν$ and the
LHC
2111.08375 [abs] [pdf]
[abstract]
by Kingman Cheung, C. J. Ouseph, and TseChun Wang.
We study the impact of non-standard neutrino interactions in the context of a
new gauge boson $Z'$ in neutral-current deep-inelastic scattering performed in
ForwArd Search ExpeRiment-$\nu$ (FASER$\nu$) and in monojet production at the
Large Hadron Collider (LHC). We simulate the neutral-current deep-inelastic
neutrino-nucleon scattering $\nu N \rightarrow \nu N$ at FASER$\nu$ in the
presence of an additional $Z'$ boson, and estimate the anticipated
sensitivities to the gauge coupling in a wide range of $Z'$ mass. At the LHC,
we study the effect of $Z'$ on monojet production, which can be enhanced in
regions with large missing transverse momenta. We then use the recent results
from ATLAS with an integrated luminosity of 139 fb$^{-1}$ to improve the limits
on the gauge coupling of $Z'$. We interpret such limits on $Z'$ gauge couplings
as bounds on effective non-standard neutrino interactions. We show that the
FASER$\rm \nu$ and the LHC results cover the medium and high energy scales,
respectively, and complement one another.
Status and Perspectives of Neutrino Physics
2111.07586 [abs] [pdf]
[abstract]
by M. Sajjad Athar, [and 18 more]Steven W. Barwick, Thomas Brunner, Jun Cao, Mikhail Danilov, Kunio Inoue, Takaaki Kajita, Marek Kowalski, Manfred Lindner, Kenneth R. Long, Nathalie Palanque-Delabrouille, Werner Rodejohann, Heidi Schellman, Kate Scholberg, Seon-Hee Seo, Nigel J. T. Smith, Walter Winter, Geralyn P. Zeller, and Renata Zukanovich Funchal [hide authors].
This review demonstrates the unique role of the neutrino by discussing in
detail the physics of and with neutrinos. We deal with neutrino sources,
neutrino oscillations, absolute masses, interactions, the possible existence of
sterile neutrinos, and theoretical implications. In addition, synergies of
neutrino physics with other research fields are found, and requirements to
continue successful neutrino physics in the future, in terms of technological
developments and adequate infrastructures, are stressed.
Probing Neutrino-Portal Dark Matter at the Forward Physics Facility
2111.05868 [abs] [pdf]
[abstract]
by Kevin J. Kelly, [and 3 more]Felix Kling, Douglas Tuckler, and Yue Zhang [hide authors].
The Forward Physics Facility (FPF), planned to operate near the ATLAS
interaction point at the LHC, offers exciting new terrain to explore neutrino
properties at TeV energy scales. It will reach an unprecedented regime for
terrestrial neutrino experiments and provide the opportunity to reveal new
physics of neutrinos at higher energy scales. We demonstrate that future
detectors at the FPF have the potential to discover new mediators that couple
predominantly to neutrinos, with masses between 0.3 and 20 GeV and small
couplings not yet probed by existing searches. Such a neutrinophilic mediator
is well motivated for addressing the origin of several neutrino-portal dark
matter candidates, including thermal freeze-out and sterile-neutrino dark
matter scenarios. Experimentally, the corresponding signatures include neutrino
charged-current scattering events associated with large missing transverse
momentum, and excessive apparent tau-neutrino events. We discuss the FPF
detector capabilities needed for this search, most importantly the hadronic
energy resolution.
Sterile Neutrino Searches with MicroBooNE: Electron Neutrino
Disappearance
2111.05793 [abs] [pdf]
[abstract]
by Peter B. Denton.
A sterile neutrino is a well motivated minimal new physics model that leaves
an imprint in neutrino oscillations. Over the last two decades, a number of
hints pointing to a sterile neutrino have emerged, many of which are pointing
near $m_4\sim1$ eV. Here we show how MicroBooNE data can be used to search for
electron neutrino disappearance using each of their four analysis channels. We
find a hint for oscillations with the highest single channel significance of
$2.4\sigma$ (using the Feldman-Cousins approach) coming from the Wire-Cell
analysis and a simplified treatment of the experimental systematics. The
preferred parameters are $\sin^2(2\theta_{14})=0.35^{+0.19}_{-0.16}$ and
$\Delta m^2_{41}=1.25^{+0.74}_{-0.39}$ eV$^2$. This region of parameter space
is in good agreement with existing hints from source experiments, is at a
similar frequency but higher mixing than indicated by reactor anti-neutrinos,
and is at the edge of the region allowed by solar neutrino data. Existing
unanalyzed data from MicroBooNE could increase the sensitivity to the
$>3\sigma$ level.
Scalable Qubit Representations of Neutrino Mixing Matrices
2111.05401 [abs] [pdf]
[abstract]
by M. J. Molewski and B. J. P. Jones.
Oscillating neutrino beams exhibit quantum coherence over distances of
thousands of kilometers. Their unambiguously quantum nature suggests an
appealing test system for direct quantum simulation. Such techniques may enable
presently analytically intractable calculations involving multi-neutrino
entanglements, such as collective neutrino oscillations in supernovae, but only
once oscillation phenomenology is properly re-expressed in the language of
quantum circuits. Here we resolve outstanding conceptual issues regarding
encoding of arbitrarily mixed neutrino flavor states in the Hilbert space of an
n-qubit quantum computer. We introduce algorithms to encode mixing and
oscillation of any number of flavor-mixed neutrinos, both with and without
CP-violation, with an efficient number of prescriptive input parameters in
terms of sub-rotations of the PMNS matrix in standard form. Examples encoded
for an IBM-Q quantum computer are shown to converge to analytic predictions
both with and without CP-violation.
Galactic rotation curves versus ultralight dark matter: A systematic
comparison with SPARC data
2111.03070 [abs] [pdf]
[abstract]
by Nitsan Bar, Kfir Blum, and Chen Sun.
We look for and place observational constraints on the imprint of ultralight
dark matter (ULDM) soliton cores in rotation-dominated galaxies. Extending
previous analyses, we find a conservative constraint which disfavors the
soliton-host halo relation found in some numerical simulations over a broad
range in the ULDM particle mass $m$. Combining the observational constraints
with theoretical arguments for the efficiency of soliton formation via
gravitational dynamical relaxation, and assuming that the soliton-halo relation
is correct, our results disfavor ULDM from comprising 100\% of the total
cosmological dark matter in the range $10^{-24}~{\rm eV}\lesssim
m\lesssim10^{-20}~{\rm eV}$. The constraints probe the ULDM fraction down to
$f\lesssim0.3$ of the total dark matter.
Non-standard interactions from the future neutrino solar sector
2111.03031 [abs] [pdf]
[abstract]
by P. Martínez-Miravé, S. Molina Sedgwick, and M. Tórtola.
The next-generation neutrino experiment JUNO will determine the solar
oscillation parameters - $\sin^2 \theta_{12}$ and $\Delta m^2_{21}$ - with
great accuracy, in addition to measuring $\sin^2\theta_{13}$, $\Delta
m^2_{31}$, and the mass ordering. In parallel, the continued study of solar
neutrinos at Hyper-Kamiokande will provide complementary measurements in the
solar sector. In this paper, we address the expected sensitivity to
non-universal and flavour-changing non-standard interactions (NSI) with
$d$-type quarks from the combination of these two future neutrino experiments.
We also show the robustness of their measurements of the solar parameters
$\sin^2 \theta_{12}$ and $\Delta m^2_{21}$ in the presence of NSI. We study the
impact of the exact experimental configuration of the Hyper-Kamiokande
detector, and conclude it is of little relevance in this scenario. Finally, we
find that the LMA-D solution is expected to be present if no additional input
from non-oscillation experiments is considered.
$pp$ Solar Neutrinos at DARWIN
2111.02421 [abs] [pdf]
[abstract]
by André de Gouvêa, [and 3 more]Emma McGinness, Ivan Martinez-Soler, and Yuber F. Perez-Gonzalez [hide authors].
The DARWIN collaboration recently argued that DARWIN (DARk matter WImp search
with liquid xenoN) can collect, via neutrino--electron scattering, a large,
useful sample of solar $pp$-neutrinos, and measure their survival probability
with sub-percent precision. We explore the physics potential of such a sample
in more detail. We estimate that, with 300 ton-years of data, DARWIN can also
measure, with the help of current solar neutrino data, the value of
$\sin^2\theta_{13}$, with the potential to exclude $\sin^2\theta_{13}=0$ close
to the three-sigma level. We explore in some detail how well DARWIN can
constrain the existence of a new neutrino mass-eigenstate $\nu_4$ that is
quasi-mass-degenerate with $\nu_1$ and find that DARWIN's sensitivity
supersedes that of all current and near-future searches for new, very light
neutrinos. In particular, DARWIN can test the hypothesis that $\nu_1$ is a
pseudo-Dirac fermion as long as the induced mass-squared difference is larger
than $10^{-13}$ eV$^2$, one order of magnitude more sensitive than existing
constraints. Throughout, we allowed for the hypotheses that DARWIN is filled
with natural xenon or $^{136}$Xe-depleted xenon.
October 2021
Anisotropies of ultrahigh-energy cosmic rays in a scenario with nearby
sources
2111.00560 [abs] [pdf]
[abstract]
by Silvia Mollerach and Esteban Roulet.
The images of ultrahigh-energy cosmic ray sources get distorted, in an energy
dependent way, by the effects of Galactic and extragalactic magnetic fields.
These deflections can also affect the observed cosmic ray spectrum, specially
when the sources are transient. We study scenarios in which one or a few nearby
extragalactic sources, such as CenA or M81/M82, provide the dominant
contribution to the cosmic ray flux above the ankle of the spectrum. We discuss
the effects of the angular dispersion induced by the turbulent extragalactic
magnetic fields, and the coherent deflections caused by the regular Galactic
magnetic field, with the associated multiple imaging of the sources. We
consider the possible contribution from those sources to the dipolar
distribution discovered by the Pierre Auger Observatory above 8 EeV, as well as
to the hot spots hinted in the observations by the Pierre Auger and Telescope
Array observatories at higher energies, taking into account the mixed nature of
the cosmic ray composition.
Model-Independent Constraints on Non-Unitary Neutrino Mixing from
High-Precision Long-Baseline Experiments
2111.00329 [abs] [pdf]
[abstract]
by Sanjib Kumar Agarwalla, [and 3 more]Sudipta Das, Alessio Giarnetti, and Davide Meloni [hide authors].
Our knowledge on the active 3$\nu$ mixing angles ($\theta_{12}$,
$\theta_{13}$, and $\theta_{23}$) and the CP phase $\delta_{\mathrm{CP}}$ is
becoming accurate day-by-day enabling us to test the unitarity of the leptonic
mixing matrix with utmost precision. Future high-precision long-baseline
experiments are going to play an important role in this direction. In this
work, we study the impact of possible non-unitary neutrino mixing (NUNM) in the
context of next-generation long-baseline experiments DUNE and T2HKK/JD+KD
having one detector in Japan (T2HK/JD) and a second detector in Korea (KD). We
estimate the sensitivities of these setups to place direct, model-independent,
and competitive constraints on various NUNM parameters. We demonstrate the
possible correlations between the NUNM parameters, $\theta_{23}$, and
$\delta_{\mathrm{CP}}$. Our numerical results obtained using only far detector
data and supported by simple approximate analytical expressions of the
oscillation probabilities in matter, reveal that JD+KD has better sensitivities
for $|\alpha_{21}|$ and $\alpha_{22}$ as compared to DUNE, due to its larger
statistics in the appearance channel and less systematic uncertainties in the
disappearance channel, respectively. For $|\alpha_{31}|$, $|\alpha_{32}|$, and
$\alpha_{33}$, DUNE gives better constraints as compared to JD+KD, due to its
larger matter effect and wider neutrino energy spectrum. For $\alpha_{11}$,
both DUNE and JD+KD give similar bounds. We also show how much the bounds on
the NUNM parameters can be improved by combining the prospective data from DUNE
and JD+KD setups. We find that due to zero-distance effects, the near detectors
alone can also constrain $\alpha_{11}$, $|\alpha_{21}|$, and $\alpha_{22}$ in
both these setups. Finally, we observe that the $\nu_\tau$ appearance sample in
DUNE can improve the constraints on $|\alpha_{32}|$ and $\alpha_{33}$.
Time variation of the atmospheric neutrino flux at dark matter detectors
2110.14723 [abs] [pdf]
[abstract]
by Yi Zhuang, Louis E. Strigari, and Rafael F. Lang.
The cosmic ray flux at the lowest energies, $\lesssim 10$ GeV, is modulated
by the solar cycle, inducing a time variation that is expected to carry over
into the atmospheric neutrino flux at these energies. Here we estimate this
time variation of the atmospheric neutrino flux at five prospective underground
locations for multi-tonne scale dark matter detectors (CJPL, Kamioka, LNGS,
SNOlab and SURF). We find that between solar minimum and solar maximum, the
normalization of the flux changes by $\sim 30\%$ at a high-latitude location
such as SURF, while it changes by a smaller amount, $\lesssim 10\%$, at LNGS. A
dark matter detector that runs for a period extending through solar cycles will
be most effective at identifying this time variation. This opens the
possibility to distinguish such neutrino-induced nuclear recoils from dark
matter-induced nuclear recoils, thus allowing for the possibility of using
timing information to break through the "neutrino floor."
TauRunner: A Public Python Program to Propagate Neutral and Charged
Leptons
2110.14662 [abs] [pdf]
[abstract]
by Ibrahim Safa, [and 5 more]Jeffrey Lazar, Alex Pizzuto, Oswaldo Vasquez, Carlos A. Argüelles, and Justin Vandenbroucke [hide authors].
In the past decade IceCube's observations have revealed a flux of
astrophysical neutrinos extending to $10^{7}~\rm{GeV}$. The forthcoming
generation of neutrino observatories promises to grant further insight into the
high-energy neutrino sky, with sensitivity reaching energies up to
$10^{12}~\rm{GeV}$. At such high energies, a new set of effects becomes
relevant, which was not accounted for in the last generation of neutrino
propagation software. Thus, it is important to develop new simulations which
efficiently and accurately model lepton behavior at this scale. We present
TauRunner a PYTHON-based package that propagates neutral and charged leptons.
TauRunner supports propagation between $10~\rm{GeV}$ and $10^{12}~\rm{GeV}$.
The package accounts for all relevant secondary neutrinos produced in
charged-current tau neutrino interactions. Additionally, tau energy losses of
taus produced in neutrino interactions is taken into account, and treated
stochastically. Finally, TauRunner is broadly adaptable to divers experimental
setups, allowing for user-specified trajectories and propagation media,
neutrino cross sections, and initial spectra.
A full parametrization of the $9\times 9$ active-sterile flavor mixing
matrix in the inverse or linear seesaw scenario of massive neutrinos
2110.12705 [abs] [pdf]
[abstract]
by He-chong Han and Zhi-zhong Xing.
The inverse and linear seesaw scenarios are two typical extensions of the
canonical seesaw mechanism, which contain much more sterile degrees of freedom
but can naturally explain the smallness of three active neutrino masses at a
sufficiently low energy scale (e.g., the TeV scale). To fully describe the
mixing among three active neutrinos, three sterile neutrinos and three extra
gauge-singlet neutral fermions in either of these two seesaw paradigms, we
present the {\it first} full parametrization of the $9\times 9$ flavor mixing
matrix in terms of 36 rotation angles and 36 CP-violating phases. The exact
inverse and linear seesaw formulas are derived, respectively; and possible
deviations of the $3\times 3$ active neutrino mixing matrix from its unitary
limit are discussed by calculating the effective Jarlskog invariants and
unitarity nonagons.
Measurement of the Coherent Elastic Neutrino-Nucleus Scattering Cross
Section on CsI by COHERENT
2110.07730 [abs] [pdf]
[abstract]
by D. Akimov, [and 75 more]P. An, C. Awe, P. S. Barbeau, B. Becker, V. Belov, I. Bernardi, M. A. Blackston, C. Bock, A. Bolozdynya, J. Browning, B. Cabrera-Palmer, D. Chernyak, E. Conley, J. Daughhetee, J. Detwiler, K. Ding, M. R. Durand, Y. Efremenko, S. R. Elliott, L. Fabris, M. Febbraro, A. Gallo Rosso, A. Galindo-Uribarri, M. P. Green, M. R. Heath, S. Hedges, D. Hoang, M. Hughes, T. Johnson, A. Khromov, A. Konovalov, E. Kozlova, A. Kumpan, L. Li, J. M. Link, J. Liu, K. Mann, D. M. Markoff, J. Mastroberti, P. E. Mueller, J. Newby, D. S. Parno, S. I. Penttila, D. Pershey, R. Rapp, H. Ray, J. Raybern, O. Razuvaeva, D. Reyna, G. C. Rich, J. Ross, D. Rudik, J. Runge, D. J. Salvat, A. M. Salyapongse, K. Scholberg, A. Shakirov, G. Simakov, G. Sinev, W. M. Snow, V. Sosnovstsev, B. Suh, R. Tayloe, K. Tellez-Giron-Flores, I. Tolstukhin, E. Ujah, J. Vanderwerp, R. L. Varner, C. J. Virtue, G. Visser, T. Wongjirad, Y. -R. Yen, J. Yoo, C. -H. Yu, and J. Zettlemoyer [hide authors].
We measured the cross section of coherent elastic neutrino-nucleus scattering
(\cevns{}) using a CsI[Na] scintillating crystal in a high flux of neutrinos
produced at the Spallation Neutron Source (SNS) at Oak Ridge National
Laboratory. New data collected before detector decommissioning has more than
doubled the dataset since the first observation of \cevns{}, achieved with this
detector. Systematic uncertainties have also been reduced with an updated
quenching model, allowing for improved precision. With these analysis
improvements, the COHERENT collaboration determined the cross section to be
$(165^{+30}_{-25})\times10^{-40}$~cm$^2$, consistent with the standard model,
giving the most precise measurement of \cevns{} yet. The timing structure of
the neutrino beam has been exploited to compare the \cevns{} cross section from
scattering of different neutrino flavors. This result places leading
constraints on neutrino non-standard interactions while testing lepton flavor
universality and measures the weak mixing angle as
$\sin^2\theta_{W}=0.220^{+0.028}_{-0.026}$ at $Q^2\approx(50\text{ MeV})^2$
Ultra-high-energy neutrino scattering in an anomalous U(1) effective
field theory
2110.07517 [abs] [pdf]
[abstract]
by Chuan-Hung Chen, Cheng-Wei Chiang, and Chun-Wei Su.
A unique characteristic of exponentially growing scattering amplitude arises
in an anomalous Abelian effective field theory when an extremely light Dirac
neutrino mass is introduced to break the symmetry. We show that the low energy
effective Lagrangian can be made explicitly gauge invariant with the help of a
nonlinear representation of the Goldstone or Stueckelberg field. We study the
peculiar feature of exponential growth in the ultra-high-energy
neutrino-nucleon inelastic scattering. It is found that the inelastic
scattering cross section is highly sensitive to the ratio of gauge coupling to
the gauge boson mass, $g_X/m_X$. When the IceCube measurement of
ultra-high-energy neutrinos, which is consistent with the standard model
prediction up to $E_\nu \sim 6$ PeV, is taken into account, the inferred
constraint on $g_X/m_X$ is more severe than that obtained from the events of
mono-lepton$+$missing transverse energy at the LHC. A muon collider with a
collision energy of $10$ TeV can be a good environment other than hadron
colliders to probe the novel effect.
Reactor antineutrino anomaly in light of recent flux model refinements
2110.06820 [abs] [pdf]
[abstract]
by C. Giunti, [and 3 more]Y. F. Li, C. A. Ternes, and Z. Xin [hide authors].
We study the status of the reactor antineutrino anomaly in light of recent
reactor flux models obtained with the conversion and summation methods. We
present a new improved calculation of the IBD yields of the standard
Huber-Mueller (HM) model and those of the new models. We show that the reactor
rates and the fuel evolution data are consistent with the predictions of the
Kurchatov Institute (KI) conversion model and with those of the Estienne-Fallot
(EF) summation model, leading to a plausible robust demise of the reactor
antineutrino anomaly. We show that the results of several goodness of fit tests
favor the KI and EF models over other models that we considered. We also
discuss the implications of the new reactor flux models for short-baseline
neutrino oscillations due to active-sterile oscillations. We show that reactor
data give upper bounds on active-sterile neutrino mixing that are not very
different for the reactor flux models under consideration and are in tension
with the large mixing required by the Gallium anomaly that has been refreshed
by the recent results of the BEST experiment.
Effect of non-unitary mixing on the mass hierarchy and CP violation
determination at the Protvino to Orca experiment
2110.02917 [abs] [pdf]
[abstract]
by Daljeet Kaur, Nafis Rezwan Khan Chowdhury, and Ushak Rahaman.
In this paper, we have estimated the neutrino mass ordering and the CP
violation sensitivity of the proposed Protvino to Orca (P2O) experiment after 6
years of data-taking. Both unitary and non-unitary $3\times 3$ neutrino mass
mixing have been considered in the simulations. A forecast analysis deriving
possible future constraints on non-unitary parameters at P2O have been
performed.
Novel constraints on neutrino physics beyond the standard model from the
CONUS experiment
2110.02174 [abs] [pdf]
[abstract]
by CONUS Collaboration, [and 12 more]H. Bonet, A. Bonhomme, C. Buck, K. Fülber, J. Hakenmüller, G. Heusser, T. Hugle, M. Lindner, W. Maneschg, T. Rink, H. Strecker, and R. Wink [hide authors].
The measurements of coherent elastic neutrino-nucleus scattering (CE$\nu$NS)
experiments have opened up the possibility to constrain neutrino physics beyond
the standard model of elementary particle physics. Furthermore, by considering
neutrino-electron scattering in the keV-energy region, it is possible to set
additional limits on new physics processes. Here, we present constraints that
are derived from CONUS germanium data on beyond the standard model (BSM)
processes like tensor and vector non-standard interactions (NSIs) in the
neutrino-quark sector, as well as light vector and scalar mediators. Thanks to
the realized low background levels in the CONUS experiment at ionization
energies below 1 keV, we are able to set the world's best limits on tensor NSIs
from CE$\nu$NS and constrain the scale of corresponding new physics to lie
above 360 GeV. For vector NSIs, the derived limits strongly depend on the
assumed ionization quenching factor within the detector material, since small
quenching factors largely suppress potential signals for both, the expected
standard model CE$\nu$NS process and the vector NSIs. Furthermore, competitive
limits on scalar and vector mediators are obtained from the CE$\nu$NS channel
at reactor-site which allow to probe coupling constants as low as
$5\cdot10^{-5}$ of low mediator masses, assuming the currently favored
quenching factor regime. The consideration of neutrino-electron scatterings
allows to set even stronger constraints for mediator masses below $\sim1$ MeV
and $\sim 10$ MeV for scalar and vector mediators, respectively.
Neutrino Oscillations through the Earth's Core
2110.01148 [abs] [pdf]
[abstract]
by Peter B. Denton and Rebekah Pestes.
Neutrinos have two properties that make them fairly unique from other known
particles: extremely low cross sections and flavor changing oscillations. With
a good knowledge of the oscillation parameters soon in hand, it will become
possible to detect low-energy atmospheric neutrinos sensitive to the forward
elastic scattering off electrons in the Earth's core providing a measurement of
the core properties and the matter effect itself. As the dynamics of the
Earth's core are complicated and in a difficult to probe environment,
additional information from upcoming neutrino experiments will provide feedback
into our knowledge of geophysics as well as useful information about exoplanet
formation and various new physics scenarios including dark matter. In addition,
we can probe the existence of the matter effect in the Earth and constrain the
non-standard neutrino interaction parameter $\epsilon_{ee}^\oplus$. We show how
DUNE's sensitivity to low-energy atmospheric neutrino oscillations can provide
a novel constraint on the density and radius of the Earth's core at the 9\%
level and the Earth's matter effect at the 5\% level. Finally, we illuminate
the physics behind low-energy atmospheric neutrino resonances in the Earth.
Search for Neutrino-Induced Neutral Current $Δ$ Radiative Decay in
MicroBooNE and a First Test of the MiniBooNE Low Energy Excess Under a
Single-Photon Hypothesis
2110.00409 [abs] [pdf]
[abstract]
by MicroBooNE collaboration, [and 187 more]P. Abratenko, R. An, J. Anthony, L. Arellano, J. Asaadi, A. Ashkenazi, S. Balasubramanian, B. Baller, C. Barnes, G. Barr, V. Basque, L. Bathe-Peters, O. Benevides Rodrigues, S. Berkman, A. Bhanderi, A. Bhat, M. Bishai, A. Blake, T. Bolton, J. Y. Book, L. Camilleri, D. Caratelli, I. Caro Terrazas, R. Castillo Fernandez, F. Cavanna, G. Cerati, Y. Chen, D. Cianci, J. M. Conrad, M. Convery, L. Cooper-Troendle, J. I. Crespo-Anadon, M. Del Tutto, S. R. Dennis, P. Detje, A. Devitt, R. Diurba, R. Dorrill, K. Duffy, S. Dytman, B. Eberly, A. Ereditato, J. J. Evans, R. Fine, G. A. Fiorentini Aguirre, R. S. Fitzpatrick, B. T. Fleming, N. Foppiani, D. Franco, A. P. Furmanski, D. Garcia-Gamez, S. Gardiner, G. Ge, S. Gollapinni, O. Goodwin, E. Gramellini, P. Green, H. Greenlee, W. Gu, R. Guenette, P. Guzowski, L. Hagaman, O. Hen, C. Hilgenberg, G. A. Horton-Smith, A. Hourlier, R. Itay, C. James, X. Ji, L. Jiang, J. H. Jo, R. A. Johnson, Y. J. Jwa, D. Kalra, N. Kamp, N. Kaneshige, G. Karagiorgi, W. Ketchum, M. Kirby, T. Kobilarcik, I. Kreslo, R. LaZur, I. Lepetic, K. Li, Y. Li, K. Lin, B. R. Littlejohn, W. C. Louis, X. Luo, K. Manivannan, C. Mariani, D. Marsden, J. Marshall, D. A. Martinez Caicedo, K. Mason, A. Mastbaum, N. McConkey, V. Meddage, T. Mettler, K. Miller, J. Mills, K. Mistry, T. Mohayai, A. Mogan, J. Moon, M. Mooney, A. F. Moor, C. D. Moore, L. Mora Lepin, J. Mousseau, M. Murphy, D. Naples, A. Navrer-Agasson, M. Nebot-Guinot, R. K. Neely, D. A. Newmark, J. Nowak, M. Nunes, O. Palamara, V. Paolone, A. Papadopoulou, V. Papavassiliou, S. F. Pate, N. Patel, A. Paudel, Z. Pavlovic, E. Piasetzky, I. Ponce-Pinto, S. Prince, X. Qian, J. L. Raaf, V. Radeka, A. Rafique, M. Reggiani-Guzzo, L. Ren, L. C. J. Rice, L. Rochester, J. Rodriguez Rondon, M. Rosenberg, M. Ross-Lonergan, G. Scanavini, D. W. Schmitz, A. Schukraft, W. Seligman, M. H. Shaevitz, R. Sharankova, J. Shi, J. Sinclair, A. Smith, E. L. Snider, M. Soderberg, S. Soldner-Rembold, P. Spentzouris, J. Spitz, M. Stancari, J. St. John, T. Strauss, K. Sutton, S. Sword-Fehlberg, A. M. Szelc, W. Tang, K. Terao, C. Thorpe, D. Totani, M. Toups, Y. -T. Tsai, M. A. Uchida, T. Usher, W. Van De Pontseele, B. Viren, M. Weber, H. Wei, Z. Williams, S. Wolbers, T. Wongjirad, M. Wospakrik, K. Wresilo, N. Wright, W. Wu, E. Yandel, T. Yang, G. Yarbrough, L. E. Yates, H. W. Yu, G. P. Zeller, J. Zennamo, and C. Zhang [hide authors].
We report results from a search for neutrino-induced neutral current (NC)
resonant $\Delta$(1232) baryon production followed by $\Delta$ radiative decay,
with a $\langle0.8\rangle$~GeV neutrino beam. Data corresponding to
MicroBooNE's first three years of operations (6.80$\times$10$^{20}$ protons on
target) are used to select single-photon events with one or zero protons and
without charged leptons in the final state ($1\gamma1p$ and $1\gamma0p$,
respectively). The background is constrained via an in-situ high-purity
measurement of NC $\pi^0$ events, made possible via dedicated $2\gamma1p$ and
$2\gamma0p$ selections. A total of 16 and 153 events are observed for the
$1\gamma1p$ and $1\gamma0p$ selections, respectively, compared to a constrained
background prediction of $20.5 \pm 3.65 \text{(sys.)} $ and $145.1 \pm 13.8
\text{(sys.)} $ events. The data lead to a bound on an anomalous enhancement of
the normalization of NC $\Delta$ radiative decay of less than $2.3$ times the
predicted nominal rate for this process at the 90% confidence level (CL). The
measurement disfavors a candidate photon interpretation of the MiniBooNE
low-energy excess as a factor of $3.18$ times the nominal NC $\Delta$ radiative
decay rate at the 94.8% CL, in favor of the nominal prediction, and represents
a greater than $50$-fold improvement over the world's best limit on
single-photon production in NC interactions in the sub-GeV neutrino energy
range
September 2021
DUNE atmospheric neutrinos: Earth Tomography
2110.00003 [abs] [pdf]
[abstract]
by Kevin J. Kelly, [and 3 more]Pedro A. N. Machado, Ivan Martinez-Soler, and Yuber F. Perez-Gonzalez [hide authors].
In this paper we show that the DUNE experiment can measure the Earth's
density profile by analyzing atmospheric neutrino oscillations. The crucial
feature that enables such measurement is the detailed event reconstruction
capability of liquid argon time projection chambers. This allows for studying
the sub-GeV atmospheric neutrino component, which bears a rich oscillation
phenomenology, strongly dependent on the matter potential sourced by the Earth.
We provide a pedagogical discussion of the MSW and parametric resonances and
their role in measuring the core and mantle densities. By performing a detailed
simulation, accounting for particle reconstruction at DUNE, nuclear physics
effects relevant to neutrino-argon interactions and several uncertainties on
the atmospheric neutrino flux, we manage to obtain a robust estimate of DUNE's
sensitivity to the Earth matter profile. We find that DUNE can measure the
total mass of the Earth at 8.4% precision with an exposure of 400~kton-year. By
accounting for previous measurements of the total mass and moment of inertia of
the Earth, the core, lower mantle and upper mantle densities can be determined
with 8.8%, 13% and 22% precision, respectively, for the same exposure. Finally,
DUNE could take atmospheric neutrino data while the beam is being commissioned
and far detector modules are up and running. For a low exposure run of
60~kton-year, which would correspond to two far detectors running for three
years, we have found that the core density could be measured by DUNE at
$\sim30\%$ precision.
Testing sterile neutrino mixing with present and future solar neutrino
data
2109.14898 [abs] [pdf]
[abstract]
by Kim Goldhagen, [and 3 more]Michele Maltoni, Shayne Reichard, and Thomas Schwetz [hide authors].
We investigate the sensitivity of solar neutrino data to mixing of sterile
neutrinos with masses $\gtrsim$ eV. For current data, we perform a
Feldman-Cousins analysis to derive a robust limit on the sterile neutrino
mixing. The solar neutrino limit excludes significant regions of the parameter
space relevant to hints from reactor and radioactive gallium source
experiments. We then study the sensitivity of upcoming solar neutrino data,
most notably elastic neutrino-electron scattering in the DARWIN and DUNE
experiments as well as coherent neutrino-nucleus scattering in DARWIN. These
high precision measurements will increase the sensitivity to sterile neutrino
mixing by about a factor of 4.5 compared to present limits. As a by-product, we
introduce a simplified solar neutrino analysis using only four data points: the
low- and high-energy $\nu_e$ survival and transition probabilities. We show
that this simplified analysis is in excellent agreement with a full solar
neutrino analysis; it is very easy to handle numerically and can be applied to
any new physics model in which the energy dependence of the $\nu_e$ transition
probabilities is not significantly modified.
Tau Neutrino Identification in Atmospheric Neutrino Oscillations Without
Particle Identification or Unitarity
2109.14576 [abs] [pdf]
[abstract]
by Peter B. Denton.
The largest tau neutrino dataset to date is IceCube's atmospheric tau
neutrino appearance dataset containing $>1,000$ tau neutrino and antineutrino
events as determined by a fit to a standard three-flavor oscillation framework.
On an event-by-event basis, however, it is impossible to know that any given
event is a tau neutrino as they are identical to either an electron neutrino
charged-current event or a neutral-current interaction of any active flavor.
Nonetheless, we conclusively show that, using only the cascade sample even
without knowledge of the oscillation parameters and without assuming that the
lepton mixing matrix is unitary, tau neutrino identification is still possible
and there is no viable scenario in which all of the tau neutrino candidates are
actually electron neutrinos. This is primarily due to the matter effect and the
tau lepton production threshold, as well as the fact that tau neutrinos are
systematically reconstructed at a lower energy than electron neutrinos due to
one or more outgoing neutrinos. This conclusively shows that it is possible for
an atmospheric neutrino oscillation experiment to confirm that $U_{\tau1}$,
$U_{\tau2}$, and $U_{\tau3}$ are not all zero even with limited particle
identification.
New oscillation and scattering constraints on the tau row matrix
elements without assuming unitarity
2109.14575 [abs] [pdf]
[abstract]
by Peter B. Denton and Julia Gehrlein.
The tau neutrino is the least well measured particle in the Standard Model.
Most notably, the tau neutrino row of the lepton mixing matrix is quite poorly
constrained when unitarity is not assumed. In this paper, we identify data sets
involving tau neutrinos that improve our understanding of the tau neutrino part
of the mixing matrix, in particular $\nu_\tau$ appearance in atmospheric
neutrinos. We present new results on the elements of the tau row leveraging
existing constraints on the electron and muon rows for the cases of unitarity
violation, with and without kinematically accessible steriles. We also show the
expected sensitivity due to upcoming experiments and demonstrate that the tau
neutrino row precision may be comparable to the muon neutrino row in a careful
combined fit.
Lorentz symmetry and high-energy neutrino astronomy
2109.13973 [abs] [pdf]
[abstract]
by Carlos A. Argüelles and Teppei Katori.
The search of violation of Lorentz symmetry, or Lorentz violation (LV), is an
active research field. The effects of LV are expected to be very small and
special systems are often used to search it. High-energy astrophysical
neutrinos offer a unique system to search signatures of LV due to the three
factors: high neutrino energy, long propagation distance, and the presence of
quantum mechanical interference. In this brief review, we introduce tests of LV
and summarize existing searches of LV using atmospheric and astrophysical
neutrinos.
Non-unitary Leptonic Flavor Mixing and CP Violation in
Neutrino-antineutrino Oscillations
2109.13622 [abs] [pdf]
[abstract]
by Yilin Wang and Shun Zhou.
If massive neutrinos are Majorana particles, then the lepton number should be
violated in nature and neutrino-antineutrino oscillations $\nu^{}_\alpha
\leftrightarrow \overline{\nu}^{}_\beta$ (for $\alpha, \beta = e, \mu, \tau$)
will definitely take place. In the present paper, we study the properties of CP
violation in neutrino-antineutrino oscillations with the non-unitary leptonic
flavor mixing matrix, which is actually a natural prediction in the canonical
seesaw model due to the mixing between light and heavy Majorana neutrinos. The
oscillation probabilities $P(\nu^{}_\alpha \to \overline{\nu}^{}_\beta)$ and
$P(\overline{\nu}^{}_\alpha \to \nu^{}_\beta)$ are derived, and the CP
asymmetries ${\cal A}^{}_{\alpha \beta} \equiv [P(\nu^{}_\alpha \to
\overline{\nu}^{}_\beta) - P(\overline{\nu}^{}_\alpha \to
\nu^{}_\beta)]/[P(\nu^{}_\alpha \to \overline{\nu}^{}_\beta) +
P(\overline{\nu}^{}_\alpha \to \nu^{}_\beta)]$ are also calculated. Taking into
account current experimental bounds on the leptonic unitarity violation, we
show that the CP asymmetries induced by the non-unitary mixing parameters can
significantly deviate from those in the limit of a unitary leptonic flavor
mixing.
Updating $ν_{3}$ lifetime from solar antineutrino spectra
2109.13272 [abs] [pdf]
[abstract]
by R. Picoreti, [and 3 more]D. Pramanik, P. C. de Holanda, and O. L. G. Peres [hide authors].
We study the production of antineutrinos from the solar neutrinos due the
Majorana neutrino decays of neutrino to antineutrino. Using the antineutrino
spectra from KamLAND and Borexino, we present newest limits on the lifetime of
$\nu_{3}$ in this scenario. We consider $\nu_{3} \rightarrow \bar{\nu}_{1} + X$
and $\nu_{3} \rightarrow \bar{\nu}_{2} + X$ channels assuming scalar or
pseudo-scalar interactions. For hierarchical mass-splittings, the limits
obtained by us are $\tau_{3}/m_{3}~\geq 7\times 10^{-5} s/eV$ and
$\tau_{3}/m_{3}~\geq 1\times 10^{-5} s/eV$ for the two channels at $90\%$ C.L.
We found that the newest bound is five orders of magnitude better than the
atmospheric and long-baseline bounds.
Diffuse Supernova Neutrino Background Search at Super-Kamiokande
2109.11174 [abs] [pdf]
[abstract]
by Super-Kamiokande Collaboration, [and 221 more]:, K. Abe, C. Bronner, Y. Hayato, K. Hiraide, M. Ikeda, S. Imaizumi, J. Kameda, Y. Kanemura, Y. Kataoka, S. Miki, M. Miura, S. Moriyama, Y. Nagao, M. Nakahata, S. Nakayama, T. Okada, K. Okamoto, A. Orii, G. Pronost, H. Sekiya, M. Shiozawa, Y. Sonoda, Y. Suzuki, A. Takeda, Y. Takemoto, A. Takenaka, H. Tanaka, S. Watanabe, T. Yano, S. Han, T. Kajita, K. Okumura, T. Tashiro, J. Xia, G. D. Megias, D. Bravo-Bergu, L. Labarga, Ll. Marti, B. Zaldivar, B. W. Pointon, F. d. M. Blaszczyk, E. Kearns, J. L. Raaf, J. L. Stone, L. Wan, T. Wester, J. Bian, N. J. Griskevich, W. R. Kropp, S. Locke, S. Mine, M. B. Smy, H. W. Sobel, V. Takhistov, J. Hill, J. Y. Kim, I. T. Lim, R. G. Park, B. Bodur, K. Scholberg, C. W. Walter, S. Cao, L. Bernard, A. Coffani, O. Drapier, S. El Hedri, A. Giampaolo, M. Gonin, Th. A. Mueller, P. Paganini, B. Quilain, T. Ishizuka, T. Nakamura, J. S. Jang, J. G. Learned, L. H. V. Anthony, D. Martin, M. Scott, A. A. Sztuc, Y. Uchida, V. Berardi, M. G. Catanesi, E. Radicioni, N. F. Calabria, L. N. Machado, G. De Rosa, G. Collazuol, F. Iacob, M. Lamoureux, M. Mattiazzi, N. Ospina, L. Ludovici, Y. Maekawa, Y. Nishimura, M. Friend, T. Hasegawa, T. Ishida, T. Kobayashi, M. Jakkapu, T. Matsubara, T. Nakadaira, K. Nakamura, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, Y. Kotsar, Y. Nakano, H. Ozaki, T. Shiozawa, A. T. Suzuki, Y. Takeuchi, S. Yamamoto, A. Ali, Y. Ashida, J. Feng, S. Hirota, T. Kikawa, M. Mori, T. Nakaya, R. A. Wendell, K. Yasutome, P. Fernandez, N. McCauley, P. Mehta, K. M. Tsui, Y. Fukuda, Y. Itow, H. Menjo, T. Niwa, K. Sato, M. Tsukada, J. Lagoda, S. M. Lakshmi, P. Mijakowski, J. Zalipska, J. Jiang, C. K. Jung, C. Vilela, M. J. Wilking, C. Yanagisawa, K. Hagiwara, M. Harada, T. Horai, H. Ishino, S. Ito, H. Kitagawa, Y. Koshio, W. Ma, N. Piplani, S. Sakai, G. Barr, D. Barrow, L. Cook, A. Goldsack, S. Samani, D. Wark, F. Nova, T. Boschi, F. Di Lodovico, J. Gao, J. Migenda, M. Taani, S. Zsoldos, J. Y. Yang, S. J. Jenkins, M. Malek, J. M. McElwee, O. Stone, M. D. Thiesse, L. F. Thompson, H. Okazawa, S. B. Kim, J. W. Seo, I. Yu, K. Nishijima, M. Koshiba, K. Iwamoto, K. Nakagiri, Y. Nakajima, N. Ogawa, M. Yokoyama, K. Martens, M. R. Vagins, M. Kuze, S. Izumiyama, T. Yoshida, M. Inomoto, M. Ishitsuka, H. Ito, T. Kinoshita, R. Matsumoto, K. Ohta, M. Shinoki, T. Suganuma, A. K. Ichikawa, K. Nakamura, J. F. Martin, H. A. Tanaka, T. Towstego, R. Akutsu, V. Gousy-Leblanc, M. Hartz, A. Konaka, P. de Perio, N. W. Prouse, S. Chen, B. D. Xu, Y. Zhang, M. Posiadala-Zezula, D. Hadley, M. O'Flaherty, B. Richards, B. Jamieson, J. Walker, A. Minamino, K. Okamoto, G. Pintaudi, S. Sano, and R. Sasaki [hide authors].
A new search for the diffuse supernova neutrino background (DSNB) flux has
been conducted at Super-Kamiokande (SK), with a $22.5\times2970$-kton$\cdot$day
exposure from its fourth operational phase IV. The new analysis improves on the
existing background reduction techniques and systematic uncertainties and takes
advantage of an improved neutron tagging algorithm to lower the energy
threshold compared to the previous phases of SK. This allows for setting the
world's most stringent upper limit on the extraterrestrial $\bar{\nu}_e$ flux,
for neutrino energies below 31.3 MeV. The SK-IV results are combined with the
ones from the first three phases of SK to perform a joint analysis using
$22.5\times5823$ kton$\cdot$days of data. This analysis has the world's best
sensitivity to the DSNB $\bar{\nu}_e$ flux, comparable to the predictions from
various models. For neutrino energies larger than 17.3 MeV, the new combined
$90\%$ C.L. upper limits on the DSNB $\bar{\nu}_e$ flux lie around $2.7$
cm$^{-2}$$\cdot$$\text{sec}^{-1}$, strongly disfavoring the most optimistic
predictions. Finally, potentialities of the gadolinium phase of SK and the
future Hyper-Kamiokande experiment are discussed.
The Forward Physics Facility: Sites, Experiments, and Physics Potential
2109.10905 [abs] [pdf]
[abstract]
by Luis A. Anchordoqui, [and 80 more]Akitaka Ariga, Tomoko Ariga, Weidong Bai, Kincso Balazs, Brian Batell, Jamie Boyd, Joseph Bramante, Mario Campanelli, Adrian Carmona, Francesco G. Celiberto, Grigorios Chachamis, Matthew Citron, Giovanni De Lellis, Albert De Roeck, Hans Dembinski, Peter B. Denton, Antonia Di Crecsenzo, Milind V. Diwan, Liam Dougherty, Herbi K. Dreiner, Yong Du, Rikard Enberg, Yasaman Farzan, Jonathan L. Feng, Max Fieg, Patrick Foldenauer, Saeid Foroughi-Abari, Alexander Friedland, Michael Fucilla, Jonathan Gall, Maria Vittoria Garzelli, Francesco Giuli, Victor P. Goncalves, Marco Guzzi, Francis Halzen, Juan Carlos Helo, Christopher S. Hill, Ahmed Ismail, Ameen Ismail, Richard Jacobsson, Sudip Jana, Yu Seon Jeong, Krzysztof Jodlowski, Kevin J. Kelly, Felix Kling, Fnu Karan Kumar, Zhen Liu, Rafal Maciula, Roshan Mammen Abraham, Julien Manshanden, Josh McFayden, Mohammed M. A. Mohammed, Pavel M. Nadolsky, Nobuchika Okada, John Osborne, Hidetoshi Otono, Vishvas Pandey, Alessandro Papa, Digesh Raut, Mary Hall Reno, Filippo Resnati, Adam Ritz, Juan Rojo, Ina Sarcevic, Christiane Scherb, Holger Schulz, Pedro Schwaller, Dipan Sengupta, Torbjörn Sjöstrand, Tyler B. Smith, Dennis Soldin, Anna Stasto, Antoni Szczurek, Zahra Tabrizi, Sebastian Trojanowski, Yu-Dai Tsai, Douglas Tuckler, Martin W. Winkler, Keping Xie, and Yue Zhang [hide authors].
The Forward Physics Facility (FPF) is a proposal to create a cavern with the
space and infrastructure to support a suite of far-forward experiments at the
Large Hadron Collider during the High Luminosity era. Located along the beam
collision axis and shielded from the interaction point by at least 100 m of
concrete and rock, the FPF will house experiments that will detect particles
outside the acceptance of the existing large LHC experiments and will observe
rare and exotic processes in an extremely low-background environment. In this
work, we summarize the current status of plans for the FPF, including recent
progress in civil engineering in identifying promising sites for the FPF and
the experiments currently envisioned to realize the FPF's physics potential. We
then review the many Standard Model and new physics topics that will be
advanced by the FPF, including searches for long-lived particles, probes of
dark matter and dark sectors, high-statistics studies of TeV neutrinos of all
three flavors, aspects of perturbative and non-perturbative QCD, and
high-energy astroparticle physics.
Potential for a precision measurement of solar $pp$ neutrinos in the
Serappis Experiment
2109.10782 [abs] [pdf]
[abstract]
by Lukas Bieger, [and 58 more]Thilo Birkenfeld, David Blum, Wilfried Depnering, Timo Enqvist, Heike Enzmann, Feng Gao, Christoph Genster, Alexandre Göttel, Christian Grewing, Maxim Gromov, Paul Hackspacher, Caren Hagner, Tobias Heinz, Philipp Kampmann, Michael Karagounis, Andre Kruth, Pasi Kuusiniemi, Tobias Lachenmaier, Daniel Liebau, Runxuan Liu, Kai Loo, Livia Ludhova, David Meyhöfer, Axel Müller, Pavithra Muralidharan, Lothar Oberauer, Rainer Othegraven, Nina Parkalian, Yatian Pei, Oliver Pilarczyk, Henning Rebber, Markus Robens, Christian Roth, Julia Sawatzki, Konstantin Schweizer, Giulio Settanta, Maciej Slupecki, Oleg Smirnov, Achim Stahl, Hans Steiger, Jochen Steinmann, Tobias Sterr, Matthias Raphael Stock, Jian Tang, Eric Theisen, Alexander Tietzsch, Wladyslaw Trzaska, Johannes van den Boom, Stefan van Waasen, Cornelius Vollbrecht, Christopher Wiebusch, Bjoern Wonsak, Michael Wurm, Christian Wysotzki, Yu Xu, Ugur Yegin, Andre Zambanini, and Jan Züfle [hide authors].
The Serappis (SEarch for RAre PP-neutrinos In Scintillator) project aims at a
precision measurement of the flux of solar $pp$ neutrinos on the few-percent
level. Such a measurement will be a relevant contribution to the study of solar
neutrino oscillation parameters and a sensitive test of the solar luminosity
constraint. The concept of Serappis relies on a small organic liquid
scintillator detector ($\sim$20 m$^3$) with excellent energy resolution
($\sim$2.5 % at 1 MeV), low internal background and sufficient shielding from
surrounding radioactivity. This can be achieved by a minor upgrade of the
OSIRIS facility at the site of the JUNO neutrino experiment in southern China.
To go substantially beyond current accuracy levels for the $pp$ flux, an
organic scintillator with ultra-low $^{14}$C levels (below $10^{-18}$) is
required. The existing OSIRIS detector and JUNO infrastructure will be
instrumental in identifying suitable scintillator materials, offering a unique
chance for a low-budget high-precision measurement of a fundamental property of
our Sun that will be otherwise hard to access.
Monte Carlo simulations of neutrino and charged lepton propagation in
the Earth with nuPyProp
2109.08198 [abs] [pdf]
[abstract]
by Sameer Patel, [and 18 more]Mary Hall Reno, Yosui Akaike, Luis Anchordoqui, Douglas Bergman, Isaac Buckland, Austin Cummings, Johannes Eser, Claire Guépin, John F. Krizmanic, Simon Mackovjak, Angela Olinto, Thomas Paul, Alex Reustle, Andrew Romero-Wolf, Fred Sarazin, Tonia Venters, Lawrence Wiencke, and Stephanie Wissel [hide authors].
An accurate modeling of neutrino flux attenuation and the distribution of
leptons they produce in transit through the Earth is an essential component to
determine neutrino flux sensitivities of underground, sub-orbital and
space-based detectors. Through neutrino oscillations over cosmic distances,
astrophysical neutrino sources are expected to produce nearly equal fluxes of
electron, muon and tau neutrinos. Of particular interest are tau neutrinos that
interact in the Earth at modest slant depths to produce $\tau$-leptons. Some
$\tau$-leptons emerge from the Earth and decay in the atmosphere to produce
extensive air showers. Future balloon-borne and satellite-based optical
Cherenkov neutrino telescopes will be sensitive to upward air showers from tau
neutrino induced $\tau$-lepton decays. We present nuPyProp, a python code that
is part of the nuSpaceSim package. nuPyProp generates look-up tables for exit
probabilities and energy distributions for $\nu_\tau\to \tau$ and $\nu_\mu\to
\mu$ propagation in the Earth. This flexible code runs with either stochastic
or continuous electromagnetic energy losses for the lepton transit through the
Earth. Current neutrino cross section models and energy loss models are
included along with templates for user input of other models. Results from
nuPyProp are compared with other recent simulation packages for neutrino and
charged lepton propagation. Sources of modeling uncertainties are described and
quantified.
SNEWPY: A Data Pipeline from Supernova Simulations to Neutrino Signals
2109.08188 [abs] [pdf]
[abstract]
by Amanda L. Baxter, [and 19 more]Segev BenZvi, Joahan Castaneda Jaimes, Alexis Coleiro, Marta Colomer Molla, Damien Dornic, Tomer Goldhagen, Anne M. Graf, Spencer Griswold, Alec Habig, Remington Hill, Shunsaku Horiuchi James P. Kneller Rafael F. Lang, Massimiliano Lincetto, Jost Migenda, Ko Nakamura, Evan O'Connor, Andrew Renshaw, Kate Scholberg, Navya Uberoi, and Arkin Worlikar [hide authors].
Current neutrino detectors will observe hundreds to thousands of neutrinos
from a Galactic supernovae, and future detectors will increase this yield by an
order of magnitude or more. With such a data set comes the potential for a huge
increase in our understanding of the explosions of massive stars, nuclear
physics under extreme conditions, and the properties of the neutrino. However,
there is currently a large gap between supernova simulations and the
corresponding signals in neutrino detectors, which will make any comparison
between theory and observation very difficult. SNEWPY is an open-source
software package which bridges this gap. The SNEWPY code can interface with
supernova simulation data to generate from the model either a time series of
neutrino spectral fluences at Earth, or the total time-integrated spectral
fluence. Data from several hundred simulations of core-collapse, thermonuclear,
and pair-instability supernovae is included in the package. This output may
then be used by an event generator such as sntools or an event rate calculator
such as SNOwGLoBES. Additional routines in the SNEWPY package automate the
processing of the generated data through the SNOwGLoBES software and collate
its output into the observable channels of each detector. In this paper we
describe the contents of the package, the physics behind SNEWPY, the
organization of the code, and provide examples of how to make use of its
capabilities.
An Altarelli Cocktail for the MiniBooNE Anomaly?
2109.08157 [abs] [pdf]
[abstract]
by Vedran Brdar and Joachim Kopp.
We critically examine a number of theoretical uncertainties affecting the
MiniBooNE short-baseline neutrino oscillation experiment in an attempt to
better understand the observed excess of electron-like events. We re-examine
the impact of fake charged current quasi-elastic (CCQE) events, the background
due to neutral current $\pi^0$ production, and the single-photon background.
For all processes, we compare the predictions of different event generators
(GENIE, GiBUU, NUANCE, and NuWro) and, for GENIE, of different tunes. Where
MiniBooNE uses data-driven background predictions, we discuss the uncertainties
affecting the relation between the signal sample and the control sample. In the
case of the single-photon background, we emphasize the uncertainties in the
radiative branching ratios of heavy hadronic resonances. We find that not even
a combination of uncertainties in different channels adding up unfavorably (an
"Altarelli cocktail") appears to be sufficient to resolve the MiniBooNE
anomaly. We finally investigate how modified background predictions affect the
fit of a $3+1$ sterile neutrino scenario. We carefully account for full
four-flavor oscillations not only in the signal, but also in the background and
control samples. We emphasize that because of the strong correlation between
MiniBooNE's $\nu_e$ and $\nu_\mu$ samples, a sterile neutrino mixing only with
$\nu_\mu$ is sufficient to explain the anomaly, even though the well-known
tension with external constraints on $\nu_\mu$ disappearance persists.
Measuring tau neutrino appearance probability via unitarity
2109.06933 [abs] [pdf]
[abstract]
by Ivan Martinez-Soler and Hisakazu Minakata.
We propose a {\em unitarity method} for determining $\tau$ neutrino
appearance probability $P(\nu_{\mu} \rightarrow \nu_{\tau})$ in long-baseline
(LBL) accelerator experiments and atmospheric neutrino observations. When
simultaneous in situ measurements of $P(\nu_{\mu} \rightarrow \nu_{\mu})$ and
$P(\nu_{\mu} \rightarrow \nu_{e})$ proceed, as is typical in the LBL
experiments, one can use unitarity to "measure" $P(\nu_{\mu} \rightarrow
\nu_{\tau})$. A theorists' toy analysis for the model-independent determination
of $P(\nu_{\mu} \rightarrow \nu_{\mu})$ and $P(\nu_{\mu} \rightarrow \nu_{e})$
is presented by using the NOvA data. It is shown in our analysis that
$\lsim$5\% (8\%) measurement of $\tau$ neutrino appearance probability in
neutrino (antineutrino) mode is possible in the peak region $1.5 \lesssim E_\nu
\lesssim 2.5$ GeV. The $\nu$SM-independent nature of determination of the
probabilities is emphasized.
Neutrino Interaction Physics in Neutrino Telescopes
2109.04430 [abs] [pdf]
[abstract]
by Teppei Katori, Juan Pablo Yanez, and Tianlu Yuan.
Neutrino telescopes can observe neutrino interactions starting at GeV
energies by sampling a small fraction of the Cherenkov radiation produced by
charged secondary particles. These experiments instrument volumes massive
enough to collect substantial samples of neutrinos up to the TeV scale as well
as small samples at the PeV scale. This unique ability of neutrino telescopes
has been exploited to study the properties of neutrino interactions across
energies that cannot be accessed with man-made beams. Here we present the
methods and results obtained by IceCube, the most mature neutrino telescope in
operation, and offer a glimpse of what the future holds in this field.
Heavy neutral leptons below the kaon mass at hodoscopic detectors
2109.03831 [abs] [pdf]
[abstract]
by Carlos A. Argüelles, Nicolò Foppiani, and Matheus Hostert.
Heavy neutral leptons ($N$) below the kaon mass are severely constrained by
cosmology and lab-based searches for their decays in flight. If $N$ interacts
via an additional force, $N\to\nu e^+e^-$ decays are enhanced and cosmological
limits can be avoided. We show that the T2K and MicroBooNE neutrino experiments
provide the best limits on the mixing of $N$ with muon-neutrinos, outperforming
past-generation experiments, previously thought to dominate. We constrain
models with electromagnetically-decaying and long-lived $N$, such as in a
transition-magnetic-moment portal and in a leptophilic axion-like particle
portal, invoked to explain the MiniBooNE excess. By considering these models as
representative examples, our results show that explanations of the MiniBooNE
excess that involve $e^+e^-$ pairs from long-lived particles are in tension
with T2K, PS191, and MicroBooNE data. Similarly, these searches also constrain
MiniBooNE explanations based on single photons due to the associated $e^+e^-$
decay mode via a virtual photon.
Constraining the neutrino mass using a multi-tracer combination of two
galaxy surveys and CMB lensing
2109.03763 [abs] [pdf]
[abstract]
by Mario Ballardini and Roy Maartens.
Measuring the total neutrino mass is one of the most exciting opportunities
available with next-generation cosmological data sets. We study the possibility
of detecting the total neutrino mass using large-scale clustering in 21cm
intensity mapping and photometric galaxy surveys, together with CMB
information. We include the scale-dependent halo bias contribution due to the
presence of massive neutrinos, and use a multi-tracer analysis in order to
reduce cosmic variance. The multi-tracer combination of an SKAO-MID 21cm
intensity map with Stage~4 CMB dramatically shrinks the uncertainty on total
neutrino mass to $\sigma(M_\nu) \simeq 45\,$meV, using only linear clustering
information ($k_{\rm max} = 0.1\, h/$Mpc) and without a prior on optical depth.
When we add to the multi-tracer the clustering information expected from LSST,
the forecast is $\sigma(M_\nu) \simeq 12\,$meV.
Mass Composition of UHECRs from $X_{\rm max}$ Distributions Recorded by
the Pierre Auger and Telescope Array Observatories
2109.03626 [abs] [pdf]
[abstract]
by Nicusor Arsene.
In this paper we infer the mass composition of the ultra high energy cosmic
rays (UHECRs) from measurements of $X_{\rm max}$ distributions recorded at the
Pierre Auger (2014) and Telescope Array (TA) (2016) Observatories, by fitting
them with all possible combinations of Monte Carlo (MC) templates from a large
set of primary species (p, He, C, N, O, Ne, Si and Fe), as predicted by
EPOS-LHC, QGSJETII-04 and Sibyll 2.1 hadronic interaction models. We use the
individual fractions of nuclei reconstructed from one experiment in each energy
interval to build equivalent MC $X_{\rm max}$ distributions, which we compare
with the experimental $X_{\rm max}$ distributions of the other experiment,
applying different statistical tests of compatibility. The results obtained
from both experiments confirm that the mass composition of the UHECRs is
dominated ($\gtrsim$$70\%$) by protons and He nuclei {in the energy range
investigated $\lg E (\rm eV)$ = [17.8--19.3] (Auger) and $\lg E \rm (eV)$ =
[18.2--19.0] (TA).} The indirect comparisons between the $X_{\rm max}$
distributions recorded by the two experiments show that the degree of
compatibility of the two datasets is good, even excellent in some high energy
intervals, especially above the ankle ($\lg E (\rm eV) \sim 18.7$). However,
our study reveals that, at low energies, further effort in data analysis is
required in order to harmonize the results of the two experiments.
Near-horizon microstructure and superradiant instability of black holes
2109.03376 [abs] [pdf]
[abstract]
by Rong-Zhen Guo, Chen Yuan, and Qing-Guo Huang.
Ultralight bosons, as important candidates of dark matter, can condense
around spinning black holes (BHs) to form long-lived ``boson clouds'' due to
superradiance instability. The boson-BH system can be observed through
gravitational wave detection and may become a new window to find traces of
ultralight bosons. In this letter we explore the effects on the superradiant
instability of BHs from the near-horizon microstructure. By introducing the
reflection parameter near a BH horizon, we derived analytical results on the
corrections to both energy levels of bosonic cloud and its characteristic
frequencies of superradiance instability. Our results imply that the evolution
of a boson-BH system and gravitational waves it emits would be influenced by
the near-horizon physics of a BH.
Fog on the horizon: a new definition of the neutrino floor for direct
dark matter searches
2109.03116 [abs] [pdf]
[abstract]
by Ciaran A. J. O'Hare.
The neutrino floor is a theoretical lower limit on WIMP-like dark matter
models that are discoverable in direct detection experiments. It is commonly
interpreted as the point at which dark matter signals become hidden underneath
a remarkably similar-looking background from neutrinos. However, it has been
known for some time that the neutrino floor is not a hard limit, but can be
pushed past with sufficient statistics. As a consequence, some have recently
advocated for calling it the "neutrino fog" instead. The downside of current
methods of deriving the neutrino floor are that they rely on arbitrary choices
of experimental exposure and energy threshold. Here we propose to define the
neutrino floor as the boundary of the neutrino fog, and develop a calculation
free from these assumptions. The technique is based on the derivative of a
hypothetical experimental discovery limit as a function of exposure, and leads
to a neutrino floor that is only influenced by the systematic uncertainties on
the neutrino flux normalisations. Our floor is broadly similar to those found
in the literature, but differs by almost an order of magnitude in the sub-GeV
range, and above 20~GeV.
Unstable Cosmic Neutrino Capture
2109.02900 [abs] [pdf]
[abstract]
by Kensuke Akita, Gaetano Lambiase, and Masahide Yamaguchi.
Future direct observations of the Cosmic Neutrino Background (C$\nu$B) have
the potential to explore a neutrino lifetime, especially in the region of the
age of the universe, $t_0=4.35\times 10^{17}\ {\rm s}$. We forecast constraints
on neutrino decay via capture of the C$\nu$B on tritium, with emphasis on the
PTOLEMY-type experiment. In addition, in some cases of invisible neutrino decay
into lighter neutrinos in the Standard Model and invisible particles, we can
constrain not only the neutrino lifetime but also the masses of the invisible
particles. For this purpose, we also formulate the energy spectra of the
lighter neutrinos produced by 2-body and 3-body decays, and those of the
electrons emitted in the process of the detection of the lighter neutrinos.
Probing neutrino decay scenarios by using the Earth matter effects on
supernova neutrinos
2109.02737 [abs] [pdf]
[abstract]
by Edwin A. Delgado, Hiroshi Nunokawa, and Alexander A. Quiroga.
The observation of Earth matter effects in the spectrum of neutrinos coming
from a next galactic core-collapse supernova (CCSN) could, in principle, reveal
if neutrino mass ordering is normal or inverted. One of the possible ways to
identify the mass ordering is through the observation of the modulations that
appear in the spectrum when neutrinos travel through the Earth before they
arrive at the detector. These features in the neutrino spectrum depend on two
factors, the average neutrino energies, and the difference between the primary
neutrino fluxes of electron and other flavors produced inside the supernova.
However, recent studies indicate that the Earth matter effect for CCSN
neutrinos is expected to be rather small and difficult to be observed by
currently operating or planned neutrino detectors mainly because of the
similarity of average energies and fluxes between electron and other flavors of
neutrinos, unless the distance to CCSN is significantly smaller than the
typically expected one, $\sim 10$ kpc. Here, we are looking towards the
possibility if the non-standard neutrino properties such as decay of neutrinos
can enhance the Earth matter effect. In this work we show that invisible
neutrino decay can potentially enhance significantly the Earth matter effect
for both $\nu_e$ and $\bar{\nu}_e$ channels at the same time for both mass
orderings, even if the neutrino spectra between electron and other flavors of
neutrinos are very similar, which is a different feature not expected for CCSN
neutrinos with standard oscillation without the decay effect.
Connecting the Extremes: A Story of Supermassive Black Holes and
Ultralight Dark Matter
2109.01678 [abs] [pdf]
[abstract]
by Hooman Davoudiasl, Peter B. Denton, and Julia Gehrlein.
The formation of ultra rare supermassive black holes (SMBHs), with masses of
$\mathcal O(10^9\,M_\odot)$, in the first billion years of the Universe remains
an open question in astrophysics. At the same time, ultralight dark matter (DM)
with mass in the vicinity of $\mathcal O(10^{-20}~\text{eV})$ has been
motivated by small scale DM distributions. Though this type of DM is
constrained by various astrophysical considerations, certain observations could
be pointing to modest evidence for it. We present a model with a confining
first order phase transition at $\sim 10$ keV temperatures, facilitating
production of $\mathcal O(10^9\,M_\odot)$ primordial SMBHs. Such a phase
transition can also naturally lead to the implied mass for a motivated
ultralight axion DM candidate, suggesting that SMBHs and ultralight DM may be
two sides of the same cosmic coin. We consider constraints and avenues to
discovery from superradiance and a modification to $N_{\rm eff}$. On general
grounds, we also expect primordial gravitational waves -- from the assumed
first order phase transition -- characterized by frequencies of $\mathcal
O(10^{-12}-10^{-9}~\text{Hz})$. This frequency regime is largely uncharted, but
could be accessible to pulsar timing arrays if the primordial gravitational
waves are at the higher end of this frequency range, as could be the case in
our assumed confining phase transition.
Low exposure long-baseline neutrino oscillation sensitivity of the DUNE
experiment
2109.01304 [abs] [pdf]
[abstract]
by DUNE Collaboration, [and 1156 more]A. Abed Abud, B. Abi, R. Acciarri, M. A. Acero, M. R. Adames, G. Adamov, D. Adams, M. Adinolfi, A. Aduszkiewicz, J. Aguilar, Z. Ahmad, J. Ahmed, B. Aimard, B. Ali-Mohammadzadeh, T. Alion, K. Allison, S. Alonso Monsalve, M. AlRashed, C. Alt, A. Alton, P. Amedo, J. Anderson, C. Andreopoulos, M. Andreotti, M. P. Andrews, F. Andrianala, S. Andringa, N. Anfimov, A. Ankowski, M. Antoniassi, M. Antonova, A. Antoshkin, S. Antusch, A. Aranda-Fernandez, L. O. Arnold, M. A. Arroyave, J. Asaadi, L. Asquith, A. Aurisano, V. Aushev, D. Autiero, M. Ayala-Torres, F. Azfar, A. Back, H. Back, J. J. Back, C. Backhouse, I. Bagaturia, L. Bagby, N. Balashov, S. Balasubramanian, P. Baldi, B. Baller, B. Bambah, F. Barao, G. Barenboim, G. J. Barker, W. Barkhouse, C. Barnes, G. Barr, J. Barranco Monarca, A. Barros, N. Barros, J. L. Barrow, A. Basharina-Freshville, A. Bashyal, V. Basque, E. Belchior, J. B. R. Battat, F. Battisti, F. Bay, J. L. Bazo Alba, J. F. Beacom, E. Bechetoille, B. Behera, L. Bellantoni, G. Bellettini, V. Bellini, O. Beltramello, N. Benekos, C. Benitez Montiel, F. Bento Neves, J. Berger, S. Berkman, P. Bernardini, R. M. Berner, S. Bertolucci, M. Betancourt, A. Betancur Rodríguez, A. Bevan, Y. Bezawada, T. J. C. Bezerra, A. Bhardwaj, V. Bhatnagar, M. Bhattacharjee, S. Bhuller, B. Bhuyan, S. Biagi, J. Bian, M. Biassoni, K. Biery, B. Bilki, M. Bishai, A. Bitadze, A. Blake, F. D. M. Blaszczyk, G. C. Blazey, E. Blucher, J. Boissevain, S. Bolognesi, T. Bolton, L. Bomben, M. Bonesini, M. Bongrand, C. Bonilla-Diaz, F. Bonini, A. Booth, F. Boran, S. Bordoni, A. Borkum, N. Bostan, P. Bour, C. Bourgeois, D. Boyden, J. Bracinik, D. Braga, D. Brailsford, A. Branca, A. Brandt, J. Bremer, C. Brew, S. J. Brice, C. Brizzolari, C. Bromberg, J. Brooke, A. Bross, G. Brunetti, M. Brunetti, N. Buchanan, H. Budd, I. Butorov, I. Cagnoli, D. Caiulo, R. Calabrese, P. Calafiura, J. Calcutt, M. Calin, S. Calvez, E. Calvo, A. Caminata, M. Campanelli, D. Caratelli, G. Carini, B. Carlus, M. F. Carneiro, P. Carniti, I. Caro Terrazas, H. Carranza, T. Carroll, J. F. Castaño Forero, A. Castillo, C. Castromonte, E. Catano-Mur, C. Cattadori, F. Cavalier, F. Cavanna, S. Centro, G. Cerati, A. Cervelli, A. Cervera Villanueva, M. Chalifour, A. Chappell, E. Chardonnet, N. Charitonidis, A. Chatterjee, S. Chattopadhyay, H. Chen, M. Chen, Y. Chen, Z. Chen, Y. Cheon, D. Cherdack, C. Chi, S. Childress, A. Chiriacescu, G. Chisnall, K. Cho, S. Choate, D. Chokheli, P. S. Chong, A. Christensen, D. Christian, G. Christodoulou, A. Chukanov, M. Chung, E. Church, V. Cicero, P. Clarke, T. E. Coan, A. G. Cocco, J. A. B. Coelho, N. Colton, E. Conley, R. Conley, J. M. Conrad, M. Convery, S. Copello, L. Cremaldi, L. Cremonesi, J. I. Crespo-Anadón, M. Crisler, E. Cristaldo, R. Cross, A. Cudd, C. Cuesta, Y. Cui, D. Cussans, O. Dalager, H. da Motta, L. Da Silva Peres, C. David, Q. David, G. S. Davies, S. Davini, J. Dawson, K. De, P. Debbins, I. De Bonis, M. P. Decowski, A. de Gouvêa, P. C. De Holanda, I. L. De Icaza Astiz, A. Deisting, P. De Jong, A. Delbart, D. Delepine, M. Delgado, A. Dell'Acqua, P. De Lurgio, J. R. T. de Mello Neto, D. M. DeMuth, S. Dennis, C. Densham, G. W. Deptuch, A. De Roeck, V. De Romeri, G. De Souza, R. Devi, R. Dharmapalan, M. Dias, F. Diaz, J. S. Díaz, S. Di Domizio, L. Di Giulio, P. Ding, L. Di Noto, C. Distefano, R. Diurba, M. Diwan, Z. Djurcic, D. Doering, S. Dolan, F. Dolek, M. J. Dolinski, L. Domine, D. Douglas, D. Douillet, G. Drake, F. Drielsma, L. Duarte, D. Duchesneau, K. Duffy, P. Dunne, H. Duyang, O. Dvornikov, D. A. Dwyer, A. S. Dyshkant, M. Eads, A. Earle, D. Edmunds, J. Eisch, L. Emberger, S. Emery, A. Ereditato, T. Erjavec, C. O. Escobar, G. Eurin, J. J. Evans, E. Ewart, A. C. Ezeribe, K. Fahey, A. Falcone, M. Fani', C. Farnese, Y. Farzan, D. Fedoseev, J. Felix, Y. Feng, E. Fernandez-Martinez, P. Fernandez Menendez, M. Fernandez Morales, F. Ferraro, L. Fields, P. Filip, F. Filthaut, A. Fiorentini, M. Fiorini, R. S. Fitzpatrick, W. Flanagan, B. Fleming, R. Flight, S. Fogarty, W. Foreman, D. V. Forero, J. Fowler, W. Fox, J. Franc, K. Francis, D. Franco, J. Freeman, J. Freestone, J. Fried, A. Friedland, F. Fuentes Robayo, S. Fuess, I. K. Furic, A. P. Furmanski, A. Gabrielli, A. Gago, H. Gallagher, A. Gallas, A. Gallego-Ros, N. Gallice, V. Galymov, E. Gamberini, T. Gamble, F. Ganacim, R. Gandhi, R. Gandrajula, F. Gao, S. Gao, D. Garcia-Gamez, M. Á. García-Peris, S. Gardiner, D. Gastler, J. Gauvreau, G. Ge, N. Geffroy, B. Gelli, A. Gendotti, S. Gent, Z. Ghorbani-Moghaddam, P. Giammaria, T. Giammaria, D. Gibin, I. Gil-Botella, S. Gilligan, C. Girerd, A. K. Giri, D. Gnani, O. Gogota, M. Gold, S. Gollapinni, K. Gollwitzer, R. A. Gomes, L. V. Gomez Bermeo, L. S. Gomez Fajardo, F. Gonnella, J. A. Gonzalez-Cuevas, D. Gonzalez-Diaz, M. Gonzalez-Lopez, M. C. Goodman, O. Goodwin, S. Goswami, C. Gotti, E. Goudzovski, C. Grace, R. Gran, E. Granados, P. Granger, A. Grant, C. Grant, D. Gratieri, P. Green, L. Greenler, J. Greer, J. Grenard, W. C. Griffith, M. Groh, J. Grudzinski, K. Grzelak, W. Gu, E. Guardincerri, V. Guarino, M. Guarise, R. Guenette, E. Guerard, M. Guerzoni, D. Guffanti, A. Guglielmi, B. Guo, V. Gupta, K. K. Guthikonda, R. Gutierrez, P. Guzowski, M. M. Guzzo, S. Gwon, C. Ha, A. Habig, H. Hadavand, R. Haenni, A. Hahn, J. Haiston, P. Hamacher-Baumann, T. Hamernik, P. Hamilton, J. Han, D. A. Harris, J. Hartnell, T. Hartnett, J. Harton, T. Hasegawa, C. Hasnip, R. Hatcher, K. W. Hatfield, A. Hatzikoutelis, C. Hayes, K. Hayrapetyan, J. Hays, E. Hazen, M. He, A. Heavey, K. M. Heeger, J. Heise, S. Henry, M. A. Hernandez Morquecho, K. Herner, V Hewes, T. Hill, S. J. Hillier, A. Himmel, E. Hinkle, L. R. Hirsch, J. Ho, J. Hoff, A. Holin, E. Hoppe, G. A. Horton-Smith, M. Hostert, A. Hourlier, B. Howard, R. Howell, I. Hristova, M. S. Hronek, J. Huang, G. Iles, N. Ilic, A. M. Iliescu, R. Illingworth, G. Ingratta, A. Ioannisian, B. Irwin, L. Isenhower, R. Itay, C. M. Jackson, V. Jain, E. James, W. Jang, B. Jargowsky, F. Jediny, D. Jena, Y. S. Jeong, C. Jesús-Valls, X. Ji, L. Jiang, S. Jiménez, A. Jipa, R. Johnson, N. Johnston, B. Jones, S. B. Jones, M. Judah, C. K. Jung, T. Junk, Y. Jwa, M. Kabirnezhad, A. Kaboth, I. Kadenko, D. Kaira, I. Kakorin, A. Kalitkina, F. Kamiya, N. Kaneshige, G. Karagiorgi, G. Karaman, A. Karcher, M. Karolak, Y. Karyotakis, S. Kasai, S. P. Kasetti, L. Kashur, N. Kazaryan, E. Kearns, P. Keener, K. J. Kelly, E. Kemp, O. Kemularia, W. Ketchum, S. H. Kettell, M. Khabibullin, A. Khotjantsev, A. Khvedelidze, D. Kim, B. King, B. Kirby, M. Kirby, J. Klein, K. Koehler, L. W. Koerner, D. H. Koh, S. Kohn, P. P. Koller, L. Kolupaeva, D. Korablev, M. Kordosky, T. Kosc, U. Kose, V. A. Kostelecký, K. Kothekar, L. Kreczko, F. Krennrich, I. Kreslo, W. Kropp, Y. Kudenko, V. A. Kudryavtsev, S. Kulagin, J. Kumar, P. Kumar, P. Kunze, N. Kurita, C. Kuruppu, V. Kus, T. Kutter, J. Kvasnicka, D. Kwak, A. Lambert, B. J. Land, C. E. Lane, K. Lang, T. Langford, M. Langstaff, J. Larkin, P. Lasorak, D. Last, C. Lastoria, A. Laundrie, G. Laurenti, A. Lawrence, I. Lazanu, R. LaZur, M. Lazzaroni, T. Le, S. Leardini, J. Learned, P. LeBrun, T. LeCompte, C. Lee, S. Y. Lee, G. Lehmann Miotto, R. Lehnert, M. A. Leigui de Oliveira, M. Leitner, L. M. Lepin, S. W. Li, T. Li, Y. Li, H. Liao, C. S. Lin, Q. Lin, S. Lin, R. A. Lineros, J. Ling, A. Lister, B. R. Littlejohn, J. Liu, S. Lockwitz, T. Loew, M. Lokajicek, I. Lomidze, K. Long, T. Lord, J. M. LoSecco, W. C. Louis, X. -G. Lu, K. B. Luk, B. Lunday, X. Luo, E. Luppi, T. Lux, V. P. Luzio, D. MacFarlane, A. A. Machado, P. Machado, C. T. Macias, J. R. Macier, A. Maddalena, A. Madera, P. Madigan, S. Magill, K. Mahn, A. Maio, A. Major, J. A. Maloney, G. Mandrioli, R. C. Mandujano, J. Maneira, L. Manenti, S. Manly, A. Mann, K. Manolopoulos, M. Manrique Plata, V. N. Manyam, L. Manzanillas, M. Marchan, A. Marchionni, W. Marciano, D. Marfatia, C. Mariani, J. Maricic, R. Marie, F. Marinho, A. D. Marino, D. Marsden, M. Marshak, C. M. Marshall, J. Marshall, J. Marteau, J. Martin-Albo, N. Martinez, D. A. Martinez Caicedo, P. Martínez Miravé, S. Martynenko, V. Mascagna, K. Mason, A. Mastbaum, F. Matichard, S. Matsuno, J. Matthews, C. Mauger, N. Mauri, K. Mavrokoridis, I. Mawby, R. Mazza, A. Mazzacane, E. Mazzucato, T. McAskill, E. McCluskey, N. McConkey, K. S. McFarland, C. McGrew, A. McNab, A. Mefodiev, P. Mehta, P. Melas, O. Mena, H. Mendez, P. Mendez, D. P. Méndez, A. Menegolli, G. Meng, M. D. Messier, W. Metcalf, T. Mettler, M. Mewes, H. Meyer, T. Miao, G. Michna, T. Miedema, V. Mikola, R. Milincic, G. Miller, W. Miller, J. Mills, C. Milne, O. Mineev, A. Minotti, O. G. Miranda, S. Miryala, C. S. Mishra, S. R. Mishra, A. Mislivec, D. Mladenov, I. Mocioiu, K. Moffat, N. Moggi, R. Mohanta, T. A. Mohayai, N. Mokhov, J. Molina, L. Molina Bueno, E. Montagna, A. Montanari, C. Montanari, D. Montanari, L. M. Montano Zetina, J. Moon, S. H. Moon, M. Mooney, A. F. Moor, D. Moreno, C. Morris, C. Mossey, E. Motuk, C. A. Moura, J. Mousseau, G. Mouster, W. Mu, L. Mualem, J. Mueller, M. Muether, S. Mufson, F. Muheim, A. Muir, M. Mulhearn, D. Munford, H. Muramatsu, S. Murphy, J. Musser, J. Nachtman, S. Nagu, M. Nalbandyan, R. Nandakumar, D. Naples, S. Narita, A. Nath, A. Navrer-Agasson, N. Nayak, M. Nebot-Guinot, K. Negishi, J. K. Nelson, J. Nesbit, M. Nessi, D. Newbold, M. Newcomer, D. Newhart, H. Newton, R. Nichol, F. Nicolas-Arnaldos, E. Niner, K. Nishimura, A. Norman, A. Norrick, R. Northrop, P. Novella, J. A. Nowak, M. Oberling, J. P. Ochoa-Ricoux, A. Olivier, A. Olshevskiy, Y. Onel, Y. Onishchuk, J. Ott, L. Pagani, S. Pakvasa, G. Palacio, O. Palamara, S. Palestini, J. M. Paley, M. Pallavicini, C. Palomares, J. L. Palomino-Gallo, W. Panduro Vazquez, E. Pantic, V. Paolone, V. Papadimitriou, R. Papaleo, A. Papanestis, S. Paramesvaran, S. Parke, E. Parozzi, Z. Parsa, M. Parvu, S. Pascoli, L. Pasqualini, J. Pasternak, J. Pater, C. Patrick, L. Patrizii, R. B. Patterson, S. J. Patton, T. Patzak, A. Paudel, B. Paulos, L. Paulucci, Z. Pavlovic, G. Pawloski, D. Payne, V. Pec, S. J. M. Peeters, E. Pennacchio, A. Penzo, O. L. G. Peres, J. Perry, D. Pershey, G. Pessina, G. Petrillo, C. Petta, R. Petti, V. Pia, F. Piastra, L. Pickering, F. Pietropaolo, R. Plunkett, R. Poling, X. Pons, N. Poonthottathil, F. Poppi, S. Pordes, J. Porter, M. Potekhin, R. Potenza, B. V. K. S. Potukuchi, J. Pozimski, M. Pozzato, S. Prakash, T. Prakash, M. Prest, S. Prince, F. Psihas, D. Pugnere, X. Qian, J. L. Raaf, V. Radeka, J. Rademacker, B. Radics, A. Rafique, E. Raguzin, M. Rai, M. Rajaoalisoa, I. Rakhno, A. Rakotonandrasana, L. Rakotondravohitra, Y. A. Ramachers, R. Rameika, M. A. Ramirez Delgado, B. Ramson, A. Rappoldi, G. Raselli, P. Ratoff, S. Raut, R. F. Razakamiandra, E. Rea, J. S. Real, B. Rebel, M. Reggiani-Guzzo, T. Rehak, J. Reichenbacher, S. D. Reitzner, H. Rejeb Sfar, A. Renshaw, S. Rescia, F. Resnati, A. Reynolds, M. Ribas, S. Riboldi, C. Riccio, G. Riccobene, L. C. J. Rice, J. Ricol, A. Rigamonti, Y. Rigaut, D. Rivera, A. Robert, L. Rochester, M. Roda, P. Rodrigues, M. J. Rodriguez Alonso, E. Rodriguez Bonilla, J. Rodriguez Rondon, S. Rosauro-Alcaraz, M. Rosenberg, P. Rosier, B. Roskovec, M. Rossella, M. Rossi, J. Rout, P. Roy, A. Rubbia, C. Rubbia, B. Russell, D. Ruterbories, A. Rybnikov, A. Saa-Hernandez, R. Saakyan, S. Sacerdoti, T. Safford, N. Sahu, P. Sala, N. Samios, O. Samoylov, M. C. Sanchez, V. Sandberg, D. A. Sanders, D. Sankey, S. Santana, M. Santos-Maldonado, N. Saoulidou, P. Sapienza, C. Sarasty, I. Sarcevic, G. Savage, V. Savinov, A. Scaramelli, A. Scarff, A. Scarpelli, H. Schellman, S. Schifano, P. Schlabach, D. Schmitz, K. Scholberg, A. Schukraft, E. Segreto, A. Selyunin, C. R. Senise, J. Sensenig, M. Seoane, A. Sergi, D. Sgalaberna, M. H. Shaevitz, S. Shafaq, M. Shamma, R. Sharankova, H. R. Sharma, R. Sharma, R. Kumar, T. Shaw, C. Shepherd-Themistocleous, A. Sheshukov, S. Shin, I. Shoemaker, D. Shooltz, R. Shrock, H. Siegel, L. Simard, F. Simon, J. Sinclair, G. Sinev, Jaydip Singh, J. Singh, L. Singh, V. Singh, R. Sipos, F. W. Sippach, G. Sirri, A. Sitraka, K. Siyeon, K. Skarpaas, A. Smith, E. Smith, P. Smith, J. Smolik, M. Smy, E. L. Snider, P. Snopok, D. Snowden-Ifft, M. Soares Nunes, H. Sobel, M. Soderberg, S. Sokolov, C. J. Solano Salinas, S. Söldner-Rembold, S. R. Soleti, N. Solomey, V. Solovov, W. E. Sondheim, M. Sorel, A. Sotnikov, J. Soto-Oton, A. Sousa, K. Soustruznik, F. Spagliardi, M. Spanu, J. Spitz, N. J. C. Spooner, K. Spurgeon, M. Stancari, L. Stanco, R. Stein, H. M. Steiner, A. F. Steklain Lisbôa, J. Stewart, B. Stillwell, J. Stock, F. Stocker, T. Stokes, M. Strait, T. Strauss, A. Stuart, J. G. Suarez, H. Sullivan, D. Summers, A. Surdo, V. Susic, L. Suter, C. M. Sutera, R. Svoboda, B. Szczerbinska, A. M. Szelc, H. A. Tanaka, B. Tapia Oregui, A. Tapper, S. Tariq, E. Tatar, R. Tayloe, A. M. Teklu, M. Tenti, K. Terao, C. A. Ternes, F. Terranova, G. Testera, T. Thakore, A. Thea, J. L. Thompson, C. Thorn, S. C. Timm, V. Tishchenko, L. Tomassetti, A. Tonazzo, D. Torbunov, M. Torti, M. Tortola, F. Tortorici, N. Tosi, D. Totani, M. Toups, C. Touramanis, R. Travaglini, J. Trevor, S. Trilov, W. H. Trzaska, Y. Tsai, Y. -T. Tsai, Z. Tsamalaidze, K. V. Tsang, N. Tsverava, S. Tufanli, C. Tull, E. Tyley, M. Tzanov, L. Uboldi, M. A. Uchida, J. Urheim, T. Usher, S. Uzunyan, M. R. Vagins, P. Vahle, G. A. Valdiviesso, R. Valentim, Z. Vallari, E. Vallazza, J. W. F. Valle, S. Vallecorsa, R. Van Berg, R. G. Van de Water, F. Varanini, D. Vargas, G. Varner, J. Vasel, S. Vasina, G. Vasseur, N. Vaughan, K. Vaziri, S. Ventura, A. Verdugo, S. Vergani, M. A. Vermeulen, M. Verzocchi, M. Vicenzi, H. Vieira de Souza, C. Vignoli, C. Vilela, B. Viren, T. Vrba, T. Wachala, A. V. Waldron, M. Wallbank, C. Wallis, H. Wang, J. Wang, L. Wang, M. H. L. S. Wang, Y. Wang, Y. Wang, K. Warburton, D. Warner, M. O. Wascko, D. Waters, A. Watson, P. Weatherly, A. Weber, M. Weber, H. Wei, A. Weinstein, D. Wenman, M. Wetstein, A. White, L. H. Whitehead, D. Whittington, M. J. Wilking, C. Wilkinson, Z. Williams, F. Wilson, R. J. Wilson, W. Wisniewski, J. Wolcott, T. Wongjirad, A. Wood, K. Wood, E. Worcester, M. Worcester, C. Wret, W. Wu, W. Wu, Y. Xiao, F. Xie, E. Yandel, G. Yang, K. Yang, T. Yang, A. Yankelevich, N. Yershov, K. Yonehara, T. Young, B. Yu, H. Yu, H. Yu, J. Yu, W. Yuan, R. Zaki, J. Zalesak, L. Zambelli, B. Zamorano, A. Zani, L. Zazueta, G. P. Zeller, J. Zennamo, K. Zeug, C. Zhang, M. Zhao, E. Zhivun, G. Zhu, E. D. Zimmerman, S. Zucchelli, J. Zuklin, V. Zutshi, and R. Zwaska [hide authors].
The Deep Underground Neutrino Experiment (DUNE) will produce world-leading
neutrino oscillation measurements over the lifetime of the experiment. In this
work, we explore DUNE's sensitivity to observe charge-parity violation (CPV) in
the neutrino sector, and to resolve the mass ordering, for exposures of up to
100 kiloton-megawatt-years (kt-MW-yr). The analysis includes detailed
uncertainties on the flux prediction, the neutrino interaction model, and
detector effects. We demonstrate that DUNE will be able to unambiguously
resolve the neutrino mass ordering at a 3$\sigma$ (5$\sigma$) level, with a 66
(100) kt-MW-yr far detector exposure, and has the ability to make strong
statements at significantly shorter exposures depending on the true value of
other oscillation parameters. We also show that DUNE has the potential to make
a robust measurement of CPV at a 3$\sigma$ level with a 100 kt-MW-yr exposure
for the maximally CP-violating values $\delta_{\rm CP}} = \pm\pi/2$.
Additionally, the dependence of DUNE's sensitivity on the exposure taken in
neutrino-enhanced and antineutrino-enhanced running is discussed. An equal
fraction of exposure taken in each beam mode is found to be close to optimal
when considered over the entire space of interest.
August 2021
Using Secondary Tau Neutrinos to Probe Heavy Dark Matter Decays in Earth
2108.13412 [abs] [pdf]
[abstract]
by Matthew Saveliev and Jeffrey Hyde.
Dark matter particles can be gravitationally trapped by celestial bodies,
motivating searches for localized annihilation or decay. If neutrinos are among
the decay products, then IceCube and other neutrino observatories could detect
them. We investigate this scenario for dark matter particles above $m_{\chi}
\gtrsim$ PeV producing tau neutrino signals, using updated modeling of dark
matter capture and thermalization. At these energies, tau neutrino regeneration
is an important effect during propagation through Earth, allowing detection at
distances far longer than one interaction length. We show how large energy loss
of tau leptons above $\sim$ PeV drives a wide range of initial energies to the
same final energy spectrum of "secondary" tau neutrinos at the detector, and we
provide an analytic approximation to the numerical results. This effect enables
an experiment to constrain decays that occur at very high energies, and we
examine the reach of the IceCube high-energy starting event (HESE) sample in
the parameter space of trapped dark matter annihilations and decays above PeV.
We find that the parameter space probed by IceCube searches would require dark
matter cross sections in tension with existing direct-detection bounds.
Energy-Dependent Neutrino Mixing Parameters at Oscillation Experiments
2108.11961 [abs] [pdf]
[abstract]
by K. S. Babu, [and 3 more]Vedran Brdar, André de Gouvêa, and Pedro A. N. Machado [hide authors].
Neutrino mixing parameters are subject to quantum corrections and hence are
scale dependent. This means that the mixing parameters associated to the
production and detection of neutrinos need not coincide since these processes
are characterized by different energy scales. We show that, in the presence of
relatively light new physics, the scale dependence of the mixing parameters can
lead to observable consequences in long-baseline neutrino oscillation
experiments, such as T2K and NOvA, and in neutrino telescopes like IceCube. We
discuss some of the experimental signatures of this scenario, including
zero-baseline flavor transitions, new sources of CP-invariance violation, and
apparent inconsistencies among measurements of mixing angles at different
experiments or oscillation channels. Finally, we present simple,
ultraviolet-complete models of neutrino masses which lead to observable running
of the neutrino mixing matrix below the weak scale.
An Improved Measurement of Neutrino Oscillation Parameters by the NOvA
Experiment
2108.08219 [abs] [pdf]
[abstract]
by M. A. Acero, [and 204 more]P. Adamson, L. Aliaga, N. Anfimov, A. Antoshkin, E. Arrieta-Diaz, L. Asquith, A. Aurisano, A. Back, C. Backhouse, M. Baird, N. Balashov, P. Baldi, B. A. Bambah, S. Bashar, K. Bays, R. Bernstein, V. Bhatnagar, D. Bhattarai, B. Bhuyan, J. Bian, J. Blair, A. C. Booth, R. Bowles, C. Bromberg, N. Buchanan, A. Butkevich, S. Calvez, T. J. Carroll, E. Catano-Mur, B. C. Choudhary, A. Christensen, T. E. Coan, M. Colo, L. Cremonesi, G. S. Davies, P. F. Derwent, P. Ding, Z. Djurcic, M. Dolce, D. Doyle, D. Dueñas Tonguino, E. C. Dukes, H. Duyang, R. Ehrlich, M. Elkins, E. Ewart, G. J. Feldman, P. Filip, J. Franc, M. J. Frank, H. R. Gallagher, R. Gandrajula, F. Gao, A. Giri, R. A. Gomes, M. C. Goodman, V. Grichine, M. Groh, R. Group, B. Guo, A. Habig, F. Hakl, A. Hall, J. Hartnell, R. Hatcher, H. Hausner, M. He, K. Heller, V. Hewes, A. Himmel, A. Holin, J. Huang, B. Jargowsky, J. Jarosz, F. Jediny, C. Johnson, M. Judah, I. Kakorin, D. M. Kaplan, A. Kalitkina, R. Keloth, O. Klimov, L. W. Koerner, L. Kolupaeva, S. Kotelnikov, R. Kralik, Ch. Kullenberg, M. Kubu, A. Kumar, C. D. Kuruppu, V. Kus, T. Lackey, K. Lang, P. Lasorak, J. Lesmeister, S. Lin, A. Lister, J. Liu, M. Lokajicek, S. Magill, M. Manrique Plata, W. A. Mann, M. L. Marshak, M. Martinez-Casales, V. Matveev, B. Mayes, D. P. Méndez, M. D. Messier, H. Meyer, T. Miao, W. H. Miller, S. R. Mishra, A. Mislivec, R. Mohanta, A. Moren, A. Morozova, W. Mu, L. Mualem, M. Muether, S. Mufson, K. Mulder, D. Naples, N. Nayak, J. K. Nelson, R. Nichol, E. Niner, A. Norman, A. Norrick, T. Nosek, H. Oh, A. Olshevskiy, T. Olson, J. Ott, J. Paley, R. B. Patterson, G. Pawloski, O. Petrova, R. Petti, D. D. Phan, R. K. Plunkett, J. C. C. Porter, A. Rafique, F. Psihas, V. Raj, M. Rajaoalisoa, B. Ramson, B. Rebel, P. Rojas, P. Roy, V. Ryabov, O. Samoylov, M. C. Sanchez, S. Sánchez Falero, P. Shanahan, A. Sheshukov, P. Singh, V. Singh, E. Smith, J. Smolik, P. Snopok, N. Solomey, A. Sousa, K. Soustruznik, M. Strait, L. Suter, A. Sutton, S. Swain, C. Sweeney, A. Sztuc, R. L. Talaga, B. Tapia Oregui, P. Tas, T. Thakore, R. B. Thayyullathil, J. Thomas, E. Tiras, J. Tripathi, J. Trokan-Tenorio, A. Tsaris, Y. Torun, J. Urheim, P. Vahle, Z. Vallari, J. Vasel, P. Vokac, T. Vrba, M. Wallbank, T. K. Warburton, M. Wetstein, D. Whittington, D. A. Wickremasinghe, S. G. Wojcicki, J. Wolcott, W. Wu, Y. Xiao, A. Yallappa Dombara, A. Yankelevich, K. Yonehara, S. Yu, Y. Yu, S. Zadorozhnyy, J. Zalesak, Y. Zhang, and R. Zwaska [hide authors].
We present new $\nu_\mu\rightarrow\nu_e$, $\nu_\mu\rightarrow\nu_\mu$,
$\overline{\nu}_\mu\rightarrow\overline{\nu}_e$, and
$\overline{\nu}_\mu\rightarrow\overline{\nu}_\mu$ oscillation measurements by
the NOvA experiment, with a 50% increase in neutrino-mode beam exposure over
the previously reported results. The additional data, combined with previously
published neutrino and antineutrino data, are all analyzed using improved
techniques and simulations. A joint fit to the $\nu_e$, $\nu_\mu$,
$\overline{\nu}_e$, and $\overline{\nu}_\mu$ candidate samples within the
3-flavor neutrino oscillation framework continues to yield a best-fit point in
the normal mass ordering and the upper octant of the $\theta_{23}$ mixing
angle, with $\Delta m^{2}_{32} = (2.41\pm0.07)\times 10^{-3}$ eV$^2$ and
$\sin^2\theta_{23} = 0.57^{+0.03}_{-0.04}$. The data disfavor combinations of
oscillation parameters that give rise to a large asymmetry in the rates of
$\nu_e$ and $\overline{\nu}_e$ appearance. This includes values of the
CP-violating phase in the vicinity of $\delta_\text{CP} = \pi/2$ which are
excluded by $>3\sigma$ for the inverted mass ordering, and values around
$\delta_\text{CP} = 3\pi/2$ in the normal ordering which are disfavored at
2$\sigma$ confidence.
Combined sensitivity of JUNO and KM3NeT/ORCA to the neutrino mass
ordering
2108.06293 [abs] [pdf]
[abstract]
by KM3NeT Collaboration, [and 277 more]S. Aiello, A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, M. Ardid, S. Ardid, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Biagi, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, M. Bouwhuis, C. Bozza, H. Brânzaş, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, D. Calvo, S. Campion, A. Capone, V. Carretero, P. Castaldi, S. Celli, M. Chabab, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, R. Coniglione, P. Coyle, A. Creusot, A. Cruz, G. Cuttone, R. Dallier, B. De Martino, I. Di Palma, A. F. Díaz, D. Diego-Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, L. A. Fusco, T. Gal, J. García Méndez, A. Garcia Soto, F. Garufi, Y. Gatelet, C. Gatius, N. Geisselbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, G. Grella, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, J. J. Hernández-Rey, J. Hofestädt, F. Huang, W. Idrissi Ibnsalih, G. Illuminati, C. W. James, M. de Jong, P. de Jong, B. J. Jung, P. Kalaczynski, O. Kalekin, U. F. Katz, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, V. Kulikovskiy, M. Labalme, R. Lahmann, M. Lamoureux, G. Larosa, C. Lastoria, A. Lazo, R. Le Breton, S. Le Stum, G. Lehaut, O. Leonardi, F. Leone, E. Leonora, N. Lessing, G. Levi, M. Lincetto, M. Lindsey Clark, T. Lipreau, C. Llorens Alvarez, F. Longhitano, D. Lopez-Coto, A. Lygda, L. Maderer, J. Majumdar, J. Mańczak, A. Margiotta, A. Marinelli, C. Markou, L. Martin, J. A. Martínez-Mora, A. Martini, F. Marzaioli, S. Mastroianni, K. W. Melis, G. Miele, P. Migliozzi, E. Migneco, P. Mijakowski, L. S. Miranda, C. M. Mollo, M. Moser, A. Moussa, R. Muller, M. Musumeci, L. Nauta, S. Navas, C. A. Nicolau, B. Nkosi, B. Ó Fearraigh, M. O'Sullivan, M. Organokov, A. Orlando, J. Palacios González, G. Papalashvili, R. Papaleo, A. M. Păun, G. E. Păvălaş, C. Pellegrino, M. Perrin-Terrin, V. Pestel, P. Piattelli, C. Pieterse, O. Pisanti, C. Poirè, V. Popa, T. Pradier, I. Probst, S. Pulvirenti, G. Quéméner, N. Randazzo, S. Razzaque, D. Real, S. Reck, G. Riccobene, A. Romanov, A. Rovelli, F. Salesa Greus, D. F. E. Samtleben, A. Sánchez Losa, M. Sanguineti, D. Santonocito, P. Sapienza, J. Schnabel, M. F. Schneider, J. Schumann, H. M. Schutte, J. Seneca, I. Sgura, R. Shanidze, A. Sharma, A. Sinopoulou, B. Spisso, M. Spurio, D. Stavropoulos, S. M. Stellacci, M. Taiuti, Y. Tayalati, H. Thiersen, S. Tingay, S. Tsagkli, V. Tsourapis, E. Tzamariudaki, D. Tzanetatos, V. Van Elewyck, G. Vasileiadis, F. Versari, D. Vivolo, G. de Wasseige, J. Wilms, R. Wojaczyński, E. de Wolf, T. Yousfi, S. Zavatarelli, A. Zegarelli, D. Zito, J. D. Zornoza, J. Zúñiga, N. Zywucka, JUNO Collaboration members, :, S. Ahmad, J. P. A. M. de André, E. Baussan, C. Bordereau, A. Cabrera, C. Cerna, G. Donchenko, E. A. Doroshkevich, M. Dracos, F. Druillole, C. Jollet, L. N. Kalousis, P. Kampmann, K. Kouzakov, A. Lokhov, B. K. Lubsandorzhiev, S. B. Lubsandorzhiev, A. Meregaglia, L. Miramonti, F. Perrot, L. F. Piñeres Rico, A. Popov, R. Rasheed, M. Settimo, K. Stankevich, H. Steiger, M. R. Stock, A. Studenikin, A. Triossi, W. Trzaska, M. Vialkov, B. Wonsak, J. Wurtz, and F. Yermia [hide authors].
This article presents the potential of a combined analysis of the JUNO and
KM3NeT/ORCA experiments to determine the neutrino mass ordering. This
combination is particularly interesting as it significantly boosts the
potential of either detector, beyond simply adding their neutrino mass ordering
sensitivities, by removing a degeneracy in the determination of $\Delta
m_{31}^2$ between the two experiments when assuming the wrong ordering. The
study is based on the latest projected performances for JUNO, and on simulation
tools using a full Monte Carlo approach to the KM3NeT/ORCA response with a
careful assessment of its energy systematics. From this analysis, a $5\sigma$
determination of the neutrino mass ordering is expected after 6 years of joint
data taking for any value of the oscillation parameters. This sensitivity would
be achieved after only 2 years of joint data taking assuming the current global
best-fit values for those parameters for normal ordering.
Probing the environments surrounding ultrahigh energy cosmic ray
accelerators and their implications for astrophysical neutrinos
2108.05512 [abs] [pdf]
[abstract]
by Marco Stein Muzio, Glennys R. Farrar, and Michael Unger.
We explore inferences on ultrahigh energy cosmic ray (UHECR) source
environments -- constrained by the spectrum and composition of UHECRs and
non-observation of extremely high energy neutrinos -- and their implications
for the observed high energy astrophysical neutrino spectrum. We find
acceleration mechanisms producing power-law CR spectra~$\propto E^{-2}$ are
compatible with UHECR data, if CRs at high rigidities are in the
quasi-ballistic diffusion regime as they escape their source environment. Both
gas-dominated and photon-dominated source environments are able to account for
UHECR observations, however photon-dominated sources give a better fit.
Additionally, gas-dominated sources are in tension with current neutrino
constraints. Accurate measurement of the neutrino flux at $\sim 10$ PeV will
provide crucial information on the viability of gas-dominated sources, as well
as whether diffusive shock acceleration is consistent with UHECR observations.
We also show that UHECR sources are able to give a good fit to the high energy
portion of the astrophysical neutrino spectrum, above $\sim$ PeV. This common
origin of UHECRs and high energy astrophysical neutrinos is natural if air
shower data is interpreted with the Sibyll2.3c hadronic interaction model,
which gives the best-fit to UHECRs and astrophysical neutrinos in the same part
of parameter space, but not for EPOS-LHC.
The potential of CMS as a high-energy neutrino scattering experiment
2108.05370 [abs] [pdf]
[abstract]
by Patrick Foldenauer, Felix Kling, and Peter Reimitz.
With its enormous number of produced neutrinos the LHC is a prime facility to
study the behaviour of high-energy neutrinos. In this paper we propose a novel
search strategy for identifying neutrino scattering via displaced appearing
jets in the high granularity calorimeter (HGCAL) of the CMS endcap in the high
luminosity run of the LHC. We demonstrate in a cut-and-count based analysis how
the enormous hadronic background can be reduced while keeping most of the
neutrino signal. This paper serves as a proof-of-principle study to illustrate
the feasibility of the first direct observation of high-energetic neutrinos
coming from $W$ decays.
Searches for light dark matter using condensed matter systems
2108.03239 [abs] [pdf]
[abstract]
by Yonatan Kahn and Tongyan Lin.
Identifying the nature of dark matter (DM) has long been a pressing question
for particle physics. In the face of ever-more-powerful exclusions and null
results from large-exposure searches for TeV-scale DM interacting with nuclei,
a significant amount of attention has shifted to lighter (sub-GeV) DM
candidates. Direct detection of the light dark matter in our galaxy by
observing DM scattering off a target system requires new approaches compared to
prior searches. Lighter DM particles have less available kinetic energy, and
achieving a kinematic match between DM and the target mandates the proper
treatment of collective excitations in condensed matter systems, such as
charged quasiparticles or phonons. In this context, the condensed matter
physics of the target material is crucial, necessitating an interdisciplinary
approach. In this review, we provide a self-contained introduction to direct
detection of keV--GeV DM with condensed matter systems. We give a brief survey
of dark matter models and basics of condensed matter, while the bulk of the
review deals with the theoretical treatment of DM-nucleon and DM-electron
interactions. We also review recent experimental developments in detector
technology, and conclude with an outlook for the field of sub-GeV DM detection
over the next decade.
First results from a search for coherent elastic neutrino-nucleus
scattering (CE$ν$NS) at a reactor site
2108.02880 [abs] [pdf]
[abstract]
by J. Colaresi, [and 6 more]J. I. Collar, T. W. Hossbach, A. R. L. Kavner, C. M. Lewis, A. E. Robinson, and K. M. Yocum [hide authors].
The deployment of a low-noise 3 kg p-type point contact germanium detector at
the Dresden-II power reactor, 8 meters from its 2.96 GW$_{th}$ core, is
described. This location provides an unprecedented (anti)neutrino flux of
8.1$\times 10^{13} ~\bar{\nu_{e}}/$cm$^{2}$s. When combined with the 0.2
keV$_{ee}$ detector threshold achieved, a first measurement of CE$\nu$NS from a
reactor source appears to be within reach. We report on the characterization
and abatement of backgrounds during initial runs, deriving improved limits on
extensions of the Standard Model involving a light vector mediator, from
preliminary data.
Searching for a Galactic component in the IceCube track-like neutrino
events
2108.01805 [abs] [pdf]
[abstract]
by Gregory S. Vance, [and 3 more]Kimberly L. Emig, Cecilia Lunardini, and Rogier A. Windhorst [hide authors].
Searches for spatial associations between high-energy neutrinos observed at
the IceCube Neutrino Observatory and known astronomical objects may hold the
key to establishing the neutrinos' origins and the origins of hadronic cosmic
rays. While extragalactic sources like the blazar TXS 0506+056 merit
significant attention, Galactic sources may also represent part of the puzzle.
Here, we explore whether open clusters and supernova remnants in the Milky Way
contribute measurably to the IceCube track-like neutrino events above 200 TeV.
By searching for positional coincidences with catalogs of known astronomical
objects, we can identify and investigate neutrino events whose origins are
potentially Galactic. We use Monte Carlo randomization together with models of
the Galactic plane in order to determine whether these coincidences are more
likely to be causal associations or random chance. In all analyses presented,
the number of coincidences detected was found to be consistent with the null
hypothesis of chance coincidence. Our results imply that the combined
contribution of Galactic open clusters and supernova remnants to the track-like
neutrino events detected at IceCube is well under 30%. This upper limit is
compatible with the results presented in other Galactic neutrino studies.
Re-examination of the Time Structure of the SN1987A Neutrino Burst Data
in Kamiokande-II
2108.01783 [abs] [pdf]
[abstract]
by Yuichi Oyama.
The seven seconds' gap in the Kamiokande-II SN1987A neutrino data is
reexamined.
July 2021
The Giant Radio Array for Neutrino Detection (GRAND) Project
2108.00032 [abs] [pdf]
[abstract]
by Kumiko Kotera.
The GRAND project aims to detect ultra-high-energy neutrinos, cosmic rays and
gamma rays, with an array of $200,000$ radio antennas over $200,000\,{\rm
km}^2$, split into $\sim 20$ sub-arrays of $\sim 10,000\,{\rm km}^2$ deployed
worldwide. The strategy of GRAND is to detect air showers above $10^{17}\,$eV
that are induced by the interaction of ultra-high-energy particles in the
atmosphere or in the Earth crust, through its associated coherent
radio-emission in the $50-200\,$MHz range. In its final configuration, GRAND
plans to reach a neutrino-sensitivity of $\sim 10^{-10}\,{\rm GeV}\,{\rm
cm}^{-2}\,{\rm s}^{-1}\,{\rm sr}^{-1}$ above $5\times 10^{17}\,$eV combined
with a sub-degree angular resolution. GRANDProto300, the 300-antenna pathfinder
array, is planned to start data-taking in 2021. It aims at demonstrating
autonomous radio detection of inclined air-showers, and study cosmic rays
around the transition between Galactic and extra-Galactic sources. We present
preliminary designs and simulation results, plans for the ongoing, staged
approach to construction, and the rich research program made possible by the
proposed sensitivity and angular resolution.
Search for neutrino non-standard interactions with ANTARES and
KM3NeT-ORCA
2107.14296 [abs] [pdf]
[abstract]
by J. J. Hernández Rey, [and 4 more]N. R. Khan Chowdhury, J. Manczak, S. Navas, and J. D. Zornoza [hide authors].
Non-standard interactions (NSIs) in the propagation of neutrinos in matter
can lead to significant deviations in neutrino oscillations expected within the
standard 3-neutrino framework. These additional interactions would result in an
anomalous flux of neutrinos observable at neutrino telescopes. The ANTARES
detector and its next-generation successor, KM3NeT, located in the abyss of the
Mediterranean Sea, have the potential to measure sub-dominant effects in
neutrino oscillations, coming from non-standard neutrino interactions. In this
contribution, a likelihood-based search for NSIs with 10 years of atmospheric
muon-neutrino data recorded with ANTARES is reported and sensitivity
projections for KM3NeT/ORCA, based on realistic detector simulations, are
shown. The bounds obtained with ANTARES in the NSI $\mu - \tau$ sector
constitute the most stringent limits up to date.
Recent Progress in Solar Atmospheric Neutrino Searches with IceCube
2107.13696 [abs] [pdf]
[abstract]
by Joshua Villarreal, Gerrit Roellinghoff, and Jeffrey Lazar.
Cosmic-rays interacting with nucleons in the solar atmosphere produce a
cascade of particles that give rise to a flux of high-energy neutrinos and
gamma-rays. Fermi has observed this gamma-ray flux; however, the associated
neutrino flux has escaped observation. In this contribution, we put forward two
strategies to detect these neutrinos, which, if seen, would push forward our
understanding of the solar atmosphere and provide a new testing ground of
neutrino properties. First, we will extend the previous analysis, which used
high-energy through-going muon events collected in the years of maximum solar
activity and yielded only flux upper limits, to include data taken during the
solar minimum from 2018 to 2020. Extending the analysis to the solar minimum is
important as the gamma-ray data collected during past solar cycles indicates a
possible enhancement in the high-energy neutrino flux. Second, we will
incorporate sub-TeV events and include contributions from all neutrino flavors.
These will improve our analysis sensitivity since the solar atmospheric
spectrum is soft and, due to oscillation, contains significant contributions of
all neutrino flavors. As we will present in this contribution, these
complementary strategies yield a significant improvement in sensitivity, making
substantial progress towards observing this flux.
Probing Secret Interactions of Astrophysical Neutrinos in the
High-Statistics Era
2107.13568 [abs] [pdf]
[abstract]
by Ivan Esteban, [and 3 more]Sujata Pandey, Vedran Brdar, and John F. Beacom [hide authors].
Do neutrinos have sizable self-interactions? They might. Laboratory
constraints are weak, so strong effects are possible in astrophysical
environments and the early universe. Observations with neutrino telescopes can
provide an independent probe of neutrino self ("secret") interactions, as the
sources are distant and the cosmic neutrino background intervenes. We define a
roadmap for making decisive progress on testing secret neutrino interactions
governed by a light mediator. This progress will be enabled by IceCube-Gen2
observations of high-energy astrophysical neutrinos. Critical to this is our
comprehensive treatment of the theory, taking into account previously neglected
or overly approximated effects, as well as including realistic detection
physics. We show that IceCube-Gen2 can realize the full potential of neutrino
astronomy for testing neutrino self-interactions, being sensitive to
cosmologically relevant interaction models. To facilitate forthcoming studies,
we release nuSIProp, a code that can also be used to study neutrino
self-interactions from a variety of sources.
JUNO's prospects for determining the neutrino mass ordering
2107.12410 [abs] [pdf]
[abstract]
by David V. Forero, [and 3 more]Stephen J. Parke, Christoph A. Ternes, and Renata Zukanovich Funchal [hide authors].
The flagship measurement of the JUNO experiment is the determination of the
neutrino mass ordering. Here we revisit its prospects to make this
determination by 2030, using the current global knowledge of the relevant
neutrino parameters as well as current information on the reactor configuration
and the critical parameters of the JUNO detector. We pay particular attention
to the non-linear detector energy response. Using the measurement of
$\theta_{13}$ from Daya Bay, but without information from other experiments, we
estimate the probability of JUNO determining the neutrino mass ordering at
$\ge$ 3$\sigma$ to be 31% by 2030. As this probability is particularly
sensitive to the true values of the oscillation parameters, especially $\Delta
m^2_{21}$, JUNO's improved measurements of $\sin^2 \theta_{12}$, $\Delta
m^2_{21}$ and $|\Delta m^2_{ee}|$, obtained after a couple of years of
operation, will allow an updated estimate of the probability that JUNO alone
can determine the neutrino mass ordering by the end of the decade. Combining
JUNO's measurement of $|\Delta m^2_{ee}|$ with other experiments in a global
fit will most likely lead to an earlier determination of the mass ordering.
Symmetry Finder applied to the 1-3 mass eigenstate exchange symmetry
2107.12086 [abs] [pdf]
[abstract]
by Hisakazu Minakata.
In a previous paper, Symmetry Finder (SF) method is proposed to find the
reparametrization symmetry of the state-exchange type in neutrino oscillation
in matter. It has been applied successfully to the 1-2 state exchange symmetry
in the DMP perturbation theory, yielding the eight symmetries. In this paper,
we apply the SF method to the atmospheric-resonance perturbation theory to
uncover the 1-3 state relabeling symmetries. The pure 1-3 state symmetry takes
the unique position that it is practically impossible to formulate in vacuum
under the conventional choice of the flavor mixing matrix. In contrast, our SF
method produces the sixteen 1-3 state exchange symmetries in matter. The
relationship between the symmetries in the original (vacuum plus matter)
Hamiltonian and the ones in the diagonalized system is discussed.
Ultralight bosons for strong gravity applications from simple Standard
Model extensions
2107.09493 [abs] [pdf]
[abstract]
by Felipe F. Freitas, [and 7 more]Carlos A. R. Herdeiro, António P. Morais, António Onofre, Roman Pasechnik, Eugen Radu, Nicolas Sanchis-Gual, and Rui Santos [hide authors].
We construct families, and concrete examples, of simple extensions of the
Standard Model that can yield ultralight {real or} complex vectors or scalars
with potential astrophysical relevance. Specifically, the mass range for these
putative fundamental bosons ($\sim 10^{-10}-10^{-20}$ eV) would lead
dynamically to both new non-black hole compact objects (bosonic stars) and new
non-Kerr black holes, with masses of $\sim M_\odot$ to $\sim 10^{10} M_\odot$,
corresponding to the mass range of astrophysical black hole candidates (from
stellar mass to supermassive). For each model, we study the properties of the
mass spectrum and interactions after spontaneous symmetry breaking, discuss its
theoretical viability and caveats, as well as some of its potential and most
relevant phenomenological implications {linking them to the} physics of compact
objects.
Searching for High-Energy Neutrinos from Core-Collapse Supernovae with
IceCube
2107.09317 [abs] [pdf]
[abstract]
by Jannis Necker.
IceCube is a cubic kilometer neutrino detector array in the Antarctic ice
that was designed to search for astrophysical, high-energy neutrinos. It has
detected a diffuse flux of astrophysical neutrinos that appears to be of
extragalactic origin. A possible contribution to this diffuse flux could stem
from core-collapse supernovae. The high-energy neutrinos could either come from
the interaction of the ejecta with a dense circumstellar medium or a jet,
emanating from the star's core, that stalls in the star's envelope. Here, we
will present results of a stacking analysis to search for this high-energy
neutrino emission from core-collapse supernovae using 7 years of $\nu_\mu$
track events from IceCube.
The Future of Solar Neutrinos
2107.08613 [abs] [pdf]
[abstract]
by G. D. Orebi Gann, [and 3 more]K. Zuber, D. Bemmerer, and A. Serenelli [hide authors].
In this article we review the current state of the field of solar neutrinos,
including flavour oscillations, non-standard effects, solar models, cross
section measurements, and the broad experimental program thus motivated and
enabled. We discuss the historical discoveries that contributed to current
knowledge, and define critical open questions to be addressed in the next
decade. We discuss the state of the art of standard solar models, including
uncertainties and problems related to the solar composition, and review
experimental and model solar neutrino fluxes, including future prospects. We
review the state of the art of the nuclear reaction data relevant for solar
fusion in the proton-proton chain and carbon-nitrogen-oxygen cycle. Finally, we
review the current and future experimental program that can address outstanding
questions in this field.
June 2021
Updated physics performance of the ESSnuSB experiment
2107.07585 [abs] [pdf]
[abstract]
by A. Alekou, [and 50 more]E. Baussan, N. Blaskovic Kraljevic, M. Blennow, M. Bogomilov, E. Bouquerel, A. Burgman, C. J. Carlile, J. Cederkall, P. Christiansen, M. Collins, E. Cristaldo Morales, L. D'Alessi, H. Danared, J. P. A. M. de André, J. P. Delahaye, M. Dracos, I. Efthymiopoulos, T. Ekelöf, M. Eshraqi, G. Fanourakis, E. Fernandez-Martinez, B. Folsom, M. Ghosh, G. Gokbulut, L. Halić, A. Kayis Topaksu, B. Kliček, K. Krhač, M. Lindroos, M. Mezzetto, M. Oglakci, T. Ohlsson, M. Olvegård, T. Ota, J. Park, G. Petkov, P. Poussot, S. Rosauro-Alcaraz, G. Stavropoulos, M. Stipčević, F. Terranova, J. Thomas, T. Tolba, R. Tsenov, G. Vankova-Kirilova, N. Vassilopoulos, E. Wildner, J. Wurtz, O. Zormpa, and Y. Zou [hide authors].
In this paper, we present the physics performance of the ESSnuSB experiment
in the standard three flavor scenario using the updated neutrino flux
calculated specifically for the ESSnuSB configuration and updated migration
matrices for the far detector. Taking conservative systematic uncertainties
corresponding to a normalization error of $5\%$ for signal and $10\%$ for
background, we find that there is $10\sigma$ $(13\sigma)$ CP violation
discovery sensitivity for the baseline option of 540 km (360 km) at
$\delta_{\rm CP} = \pm 90^\circ$. The corresponding fraction of $\delta_{\rm
CP}$ for which CP violation can be discovered at more than $5 \sigma$ is
$70\%$. Regarding CP precision measurements, the $1\sigma$ error associated
with $\delta_{\rm CP} = 0^\circ$ is around $5^\circ$ and with $\delta_{\rm CP}
= -90^\circ$ is around $14^\circ$ $(7^\circ)$ for the baseline option of 540 km
(360 km). For hierarchy sensitivity, one can have $3\sigma$ sensitivity for 540
km baseline except $\delta_{\rm CP} = \pm 90^\circ$ and $5\sigma$ sensitivity
for 360 km baseline for all values of $\delta_{\rm CP}$. The octant of
$\theta_{23}$ can be determined at $3 \sigma$ for the values of: $\theta_{23} >
51^\circ$ ($\theta_{23} < 42^\circ$ and $\theta_{23} > 49^\circ$) for baseline
of 540 km (360 km). Regarding measurement precision of the atmospheric mixing
parameters, the allowed values at $3 \sigma$ are: $40^\circ < \theta_{23} <
52^\circ$ ($42^\circ < \theta_{23} < 51.5^\circ$) and $2.485 \times 10^{-3}$
eV$^2 < \Delta m^2_{31} < 2.545 \times 10^{-3}$ eV$^2$ ($2.49 \times 10^{-3}$
eV$^2 < \Delta m^2_{31} < 2.54 \times 10^{-3}$ eV$^2$) for the baseline of 540
km (360 km).
July 2021
Multimessenger Analysis Strategy for Core-Collapse Supernova Search:
Gravitational Waves and Low-energy Neutrinos
2107.02050 [abs] [pdf]
[abstract]
by Odysse Halim, [and 6 more]Claudio Casentini, Marco Drago, Viviana Fafone, Kate Scholberg, Carlo Francesco Vigorito, and Giulia Pagliaroli [hide authors].
Core-collapse supernovae are fascinating astrophysical objects for
multimessenger studies. Gravitational waves (GWs) are expected to play a role
in the supernova explosion mechanism, but their modelling is also challenging
due to the stochastic nature of the dynamics and the vast possible progenitors,
and moreover, the GW detection from these objects is still elusive with the
already advanced detectors. Low-energy neutrinos will be emitted enormously
during the core-collapse explosion and can help for the gravitational wave
counterpart search. In this work we develop a multi-messenger strategy to
search for such astrophysical objects by exploiting a global network of both
low-energy neutrino and gravitational wave detectors. First, we discuss how to
improve the detection potential of the neutrino sub-network by exploiting the
temporal behaviour of a neutrino burst from a core-collapse supernova. We show
that with the proposed approach neutrino detectors can gain at least $10\%$ of
detection efficiency at the distance where their efficiency drops. Then, we
combine the information provided by GW and neutrino in a multimessenger
strategy. In particular, we obtain an increase of the probability to detect the
GW signal from a CCSN at $60$ kpc from zero when using only GW analysis to
$\sim 33\%$ with our combined GW-$\nu$ approach.
Keywords: multimessenger, supernova, core-collapse, low-energy neutrino,
gravitational wave.
Sensitivity to light sterile neutrino mixing parameters with KM3NeT/ORCA
2107.00344 [abs] [pdf]
[abstract]
by S. Aiello, [and 247 more]A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Biagi, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, M. Bouwhuis, C. Bozza, H. Brânzaş, F. Bretaudeau, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, D. Calvo, S. Campion, A. Capone, V. Carretero, P. Castaldi, S. Celli, M. Chabab, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Mollac, R. Coniglione, P. Coyle, A. Creusot, A. Cruz, G. Cuttone, R. Dallier, B. De Martino, M. De Palma, I. Di Palma, A. F. Díaz, D. Diego-Tortosan, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dorr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, D. Elsaesser, A. Enzenhofer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, L. A. Fusco, T. Gal, J. Garcıa Mendez, A. Garcia Soto, F. Garufi, Y. Gatelet, N. Geisselbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, G. Grella, D. Guderian, C. Guid, M. Gutierrez, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, J. J. Hernandez-Rey, J. Hofestadt, F. Huang, W. Idrissi Ibnsalih, G. Illuminati, C. W. James, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczynski, O. Kalekin, U. F. Katz, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, V. Kulikovskiy, R. Lahmann, M. Lamoureux, G. Lara, G. Larosa, C. Lastoria, R. Le Breton, S. Le Stum, O. Leonardi, F. Leone, E. Leonora, N. Lessing, G. Levi, M. Lincetto, M. Lindsey Clark, T. Lipreau, F. Longhitano, D. Lopez-Coto, A. Lygda, L. Maderer, J. Mańczak, K. Mannheim, A. Margiotta, A. Marinelli, C. Markou, L. Martin, J. A. Martínez-Mora, A. Martini, F. Marzaioli, S. Mastroianni, K. W. Melis, G. Miele, P. Migliozzi, E. Migneco, P. Mijakowski, L. S. Miranda, C. M. Mollo, M. Moser, A. Moussa, R. Muller, M. Musumeci, L. Nauta, S. Navas, C. A. Nicolau, B. Nkosi, B. Ó Fearraigh, M. O'Sullivan, M. Organokov, A. Orlando, J. Palacios González, G. Papalashvili, R. Papaleo, C. Pastore, A. M. Păun, G. E. Păv ălaş, C. Pellegrino, S. Peña Martínez, M. Perrin-Terrin, V. Pestel, P. Piattelli, C. Pieterse, O. Pisanti, C. Poirè, V. Pontoriere, V. Popa, T. Pradier, I. Probst, G. Pühlhofer, S. Pulvirenti, N. Randazzo, S. Razzaque, D. Real, S. Reck, G. Riccobene, A. Romanov, A. Rovelli, F. Salesa Greus, D. F. E. Samtleben, A. Sánchez Losa, M. Sanguineti, A. Santangelo, D. Santonocito, P. Sapienza, J. Schnabel, M. F. Schneider, J. Schumann, H. M. Schutte, J. Seneca, I. Sgura, R. Shanidze, A. Sharma, A. Sinopoulou, B. Spisso, M. Spurio, D. Stavropoulos, S. M. Stellacci, M. Taiuti, F. Tatone, Y. Tayalati, T. Thakore, H. Thiersen, S. Tingay, S. Tsagkli, V. Tsourapis, E. Tzamariudaki, D. Tzanetatos, V. Van Elewyck, G. Vasileiadis, F. Versari, D. Vivolo, G. de Wasseige, J. Wilms, R. Wojaczyński, E. de Wolf, T. Yousfi, S. Zavatarelli, A. Zegarelli, D. Zito, J. D. Zornoza, J. Zúñiga, and N. Zywucka [hide authors].
KM3NeT/ORCA is a next-generation neutrino telescope optimised for atmospheric
neutrino oscillations studies. In this paper, the sensitivity of ORCA to the
presence of a light sterile neutrino in a 3+1 model is presented. After three
years of data taking, ORCA will be able to probe the active-sterile mixing
angles $\theta_{14}$, $\theta_{24}$, $\theta_{34}$ and the effective angle
$\theta_{\mu e}$, over a broad range of mass squared difference $\Delta
m^2_{41} \sim [10^{-5}, 10]$ $\rm{eV}^2$, allowing to test the eV-mass sterile
neutrino hypothesis as the origin of short baseline anomalies, as well as
probing the hypothesis of a very light sterile neutrino, not yet constrained by
cosmology. ORCA will be able to explore a relevant fraction of the parameter
space not yet reached by present measurements.
June 2021
Model-independent test of T violation in neutrino oscillations
2106.16099 [abs] [pdf]
[abstract]
by Thomas Schwetz and Alejandro Segarra.
We propose a method to establish time reversal symmetry violation at future
neutrino oscillation experiments in a largely model-independent way. We
introduce a general parametrization of flavour transition probabilities which
holds under weak assumptions and covers a large class of new-physics scenarios.
This can be used to search for the presence of T-odd components in the
transition probabilities by comparing data at different baselines but at the
same neutrino energies. We show that this test can be performed already with
experiments at three different baselines and might be feasible with experiments
under preparation/consideration.
Exploring SMEFT Induced Non-Standard Interactions from COHERENT to
Neutrino Oscillations
2106.15800 [abs] [pdf]
[abstract]
by Yong Du, [and 4 more]Hao-Lin Li, Jian Tang, Sampsa Vihonen, and Jiang-Hao Yu [hide authors].
We investigate the prospects of next-generation neutrino oscillation
experiments DUNE, T2HK and JUNO including TAO within Standard Model Effective
Field Theory (SMEFT). We also re-interpret COHERENT data in this framework.
Considering both charged and neutral current neutrino Non-Standard Interactions
(NSIs), we analyse dimension-6 SMEFT operators and derive lower bounds to UV
scale $\Lambda$. The most powerful probe is obtained on ${\cal
O}_{{ledq}_{1211}}$ with $\Lambda \gtrsim$ 450 TeV due to the electron neutrino
sample in T2HK near detector. We find DUNE and JUNO to be complementary to T2HK
in exploring different subsets of SMEFT operators at about 25 TeV. We conclude
that near detectors play a significant role in each experiment. We also find
COHERENT with CsI and LAr targets to be sensitive to new physics up to
$\sim$900 GeV.
Testing non-standard neutrino interactions in (anti)-electron neutrino
disappearance experiments
2106.15725 [abs] [pdf]
[abstract]
by Mariano Chaves, Orlando Luis Goulart Peres, and Pedro Cunha de Holanda.
We search for scalar and tensor non-standard interactions using
(anti)-electron neutrino disappearance in oscillation data. We found a slight
preference for non-zero CP violation, coming from both tensor and scalar
interactions. The preference for CP violation is lead by Daya Bay low-energy
data with a significance that reaches $\sim1.7\sigma$ in the global analysis
(and $\sim2.1\sigma$ when considering only medium baseline reactors data)
compared to the standard neutrino oscillation scenario.
On the most constraining cosmological neutrino mass bounds
2106.15267 [abs] [pdf]
[abstract]
by Eleonora Di Valentino, Stefano Gariazzo, and Olga Mena.
We present here up-to-date neutrino mass limits exploiting the most recent
cosmological data sets. By making use of the Cosmic Microwave Background
temperature fluctuation and polarization measurements, Supernovae Ia luminosity
distances, Baryon Acoustic Oscillation observations and determinations of the
growth rate parameter, we are able to set the most constraining bound to date,
$\sum m_\nu<0.09$ eV at $95\%$~CL. This very tight limit is obtained without
the assumption of any prior on the value of the Hubble constant and highly
compromises the viability of the inverted mass ordering as the underlying
neutrino mass pattern in nature. The results obtained here further strengthen
the case for very large multitracer spectroscopic surveys as unique
laboratories for cosmological relics, such as neutrinos: that would be the case
of the Dark Energy Spectroscopic Instrument (DESI) survey and of the Euclid
mission.
Resonance refraction and neutrino oscillations
2106.13829 [abs] [pdf]
[abstract]
by Alexei Y. Smirnov and Victor B. Valera.
The refraction index and matter potential depend on neutrino energy and this
dependence has a resonance character associated to the production of the
mediator in the $s-$channel. For light mediators and light particles of medium
(background) the resonance can be realized at energies accessible to laboratory
experiments. We study properties of the energy dependence of the potential for
different C-asymmetries of background. Interplay of the background potential
and the vacuum term leads to (i) bump in the oscillation probability in the
resonance region, (ii) dip related to the MSW resonance in the background,
(iii) substantial deviation of the effective $\Delta m^2$ above the resonance
from the low energy value, etc. We considered generation of mixing in the
background. Interactions with background shifts the energy of usual MSW
resonance and produces new MSW resonances. Searches of the background effects
allow us to put bounds on new interactions of neutrinos and properties of the
background. We show that explanation of the MiniBooNE excess, as the bump due
to resonance refraction, is excluded.
Parameter symmetries of neutrino oscillations in vacuum, matter, and
approximation schemes
2106.12436 [abs] [pdf]
[abstract]
by Peter B. Denton and Stephen J. Parke.
Expressions for neutrino oscillations contain a high degree of symmetry, but
typical forms for the oscillation probabilities mask these symmetries of the
oscillation parameters. We elucidate the $2^7$ parameter symmetries of the
vacuum parameters and draw connections to the choice of definitions of the
parameters as well as interesting degeneracies. We also show that in the
presence of matter an \emph{additional} set of $2^7$ parameter symmetries exist
of the matter parameters. Due to the complexity of the exact expressions for
neutrino oscillations in matter, numerous approximations have been developed;
we show that under certain assumptions, approximate expressions have at most
$2^6$ additional parameter symmetries of the matter parameters. We also include
one parameter symmetry related to the LMA-Dark degeneracy that holds under the
assumption of CPT invariance; this adds one additional factor of two to all of
the above cases. Explicit, non-trivial examples are given of how physical
observables in neutrino oscillations, such as the probabilities, CP violation,
the position of the solar and atmospheric resonance, and the effective $\Delta
m^2$'s for disappearance probabilities, are invariant under all of the above
symmetries. We investigate which of these parameter symmetries apply to
numerous approximate expressions in the literature and show that a more careful
consideration of symmetries improves the precision of approximations.
Symmetry Finder: A method for hunting symmetry in neutrino oscillation
2106.11472 [abs] [pdf]
[abstract]
by Hisakazu Minakata.
Symmetry in neutrino oscillation serves for a better understanding of the
physical properties of the phenomenon. We present a systematic way of finding
symmetry in neutrino oscillation, which we call Symmetry Finder (SF). By
extending the known framework in vacuum into a matter environment, we derive
the SF equation, a powerful machinery for identifying symmetry in the system.
After learning lessons on symmetry in the Zaglauer-Schwarzer system with a
matter equivalent of the vacuum symmetry, we apply the SF method to the Denton
et al. (DMP) perturbation theory to first order. We show that the method is so
powerful that we uncover the eight reparametrization symmetries with the $1
\leftrightarrow 2$ state exchange in DMP, denoted as IA, IB, $\cdot \cdot
\cdot$, IVB, all new except for IA. The transformations consist of the both
fundamental and dynamical variables, indicating their equal importance. It is
also shown that all the symmetries discussed in this paper can be understood as
the Hamiltonian symmetries, which ensures their all-order validity and
applicability to varying density matter.
A deuterated liquid scintillator for supernova neutrino detection
2106.10927 [abs] [pdf]
[abstract]
by Bhavesh Chauhan, Basudeb Dasgupta, and Vivek Datar.
For the next galactic supernova, operational neutrino telescopes will measure
the neutrino flux several hours before their optical counterparts. Existing
detectors, relying mostly on charged current interactions, are mostly sensitive
to $\bar{\nu}_e$ and to a lesser extent to $\nu_e$. In order to measure the
flux of other flavors
($\nu_{\mu},\bar{\nu}_{\mu},\nu_{\tau},\text{and}~\bar{\nu}_{\tau}$), we need
to observe their neutral current interactions with the detector. Such a
measurement is not only crucial for overall normalization of the supernova
neutrino flux but also for understanding the intricate neutrino oscillation
physics. A deuterium based detector will be sensitive to all neutrino flavors.
In this paper, we propose a 1 kton deuterated liquid scintillator (DLS) based
detector that will see about 435 neutral current events and 170 (108) charged
current $\nu_e$ ($\bar{\nu}_e$) events from a fiducial supernova at a distance
of 10 kpc from Earth. We explore the possibility of extracting spectral
information from the neutral current channel
$\overset{\scriptscriptstyle(-)}{\nu} d \rightarrow
\overset{\scriptscriptstyle(-)}{\nu}np$ by measuring the quenched kinetic
energy of the proton in the final state, where the neutron in the final state
is tagged and used to reduce backgrounds. We also discuss the secondary
interactions of the recoil neutrons in the detector.
Neutrino As The Dark Force
2106.08339 [abs] [pdf]
[abstract]
by Nicholas Orlofsky and Yue Zhang.
We point out a novel role for the Standard Model neutrino in dark matter
phenomenology where the exchange of neutrinos generates a long-range potential
between dark matter particles. The resulting dark matter self interaction could
be sufficiently strong to impact small-scale structure formation, without the
need of any dark force carrier. This is a generic feature of theories where
dark matter couples to the visible sector through the neutrino portal. It is
highly testable with improved decay rate measurements at future $Z$, Higgs, and
$\tau$ factories, as well as precision cosmology.
All-flavor constraints on nonstandard neutrino interactions and
generalized matter potential with three years of IceCube DeepCore data
2106.07755 [abs] [pdf]
[abstract]
by IceCube Collaboration, [and 373 more]R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, R. An, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, Y. Ashida, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, V. Basu, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Borowka, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, F. Bradascio, J. Braun, S. Bron, J. Brostean-Kaiser, S. Browne, A. Burgman, R. S. Busse, M. A. Campana, C. Chen, D. Chirkin, K. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, P. Dave, C. De Clercq, J. J. DeLaunay, H. Dembinski, K. Deoskar, S. De Ridder, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, S. Dharani, A. Diaz, J. C. Díaz-Vélez, H. Dujmovic, M. Dunkman, M. A. DuVernois, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, A. R. Fazely, S. Fiedlschuster, A. T. Fienberg, K. Filimonov, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, A. Garcia, S. Garrappa, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glauch, T. Glüsenkamp, A. Goldschmidt, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, S. Griswold, M. Gündüz, C. Günther, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, M. Ha Minh, K. Hanson, J. Hardin, A. A. Harnisch, A. Haungs, S. Hauser, D. Hebecker, K. Helbing, F. Henningsen, E. C. Hettinger, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, T. Hoinka, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, B. J. P. Jones, R. Joppe, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, K. Kin, T. Kintscher, J. Kiryluk, S. R. Klein, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, N. Kurahashi, A. Kyriacou, N. Lad, C. Lagunas Gualda, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, J. W. Lee, K. Leonard, A. Leszczyńska, Y. Li, M. Lincetto, Q. R. Liu, M. Liubarska, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, S. Mancina, I. C. Mariş, R. Maruyama, K. Mase, T. McElroy, F. McNally, K. Meagher, A. Medina, M. Meier, S. Meighen-Berger, J. Merz, J. Micallef, D. Mockler, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, R. Naab, R. Nagai, U. Naumann, J. Necker, L. V. Nguyên, H. Niederhausen, M. U. Nisa, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, M. Oehler, A. Olivas, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, L. Paul, C. Pérez de los Heros, S. Philippen, D. Pieloth, S. Pieper, M. Pittermann, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, P. B. Price, B. Pries, G. T. Przybylski, C. Raab, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, A. Rehman, R. Reimann, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, J. Saffer, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Scharf, M. Schaufel, H. Schieler, P. Schlunder, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, S. Sclafani, D. Seckel, S. Seunarine, A. Sharma, S. Shefali, M. Silva, B. Skrzypek, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, C. Spannfellner, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, F. Tenholt, S. Ter-Antonyan, A. Terliuk, S. Tilav, F. Tischbein, K. Tollefson, L. Tomankova, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, C. F. Turley, J. P. Twagirayezu, B. Ty, M. A. Unland Elorrieta, N. Valtonen-Mattila, J. Vandenbroucke, N. van Eijndhoven, D. Vannerom, J. van Santen, S. Verpoest, M. Vraeghe, C. Walck, A. Wallace, T. B. Watson, C. Weaver, P. Weigel, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, B. J. Whelan, N. Whitehorn, C. H. Wiebusch, D. R. Williams, M. Wolf, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, Y. Xu, J. P. Yanez, S. Yoshida, S. Yu, T. Yuan, and Z. Zhang [hide authors].
We report constraints on nonstandard neutrino interactions (NSI) from the
observation of atmospheric neutrinos with IceCube, limiting all individual
coupling strengths from a single dataset. Furthermore, IceCube is the first
experiment to constrain flavor-violating and nonuniversal couplings
simultaneously. Hypothetical NSI are generically expected to arise due to the
exchange of a new heavy mediator particle. Neutrinos propagating in matter
scatter off fermions in the forward direction with negligible momentum
transfer. Hence the study of the matter effect on neutrinos propagating in the
Earth is sensitive to NSI independently of the energy scale of new physics. We
present constraints on NSI obtained with an all-flavor event sample of
atmospheric neutrinos based on three years of IceCube DeepCore data. The
analysis uses neutrinos arriving from all directions, with reconstructed
energies between 5.6 GeV and 100 GeV. We report constraints on the individual
NSI coupling strengths considered singly, allowing for complex phases in the
case of flavor-violating couplings. This demonstrates that IceCube is sensitive
to the full NSI flavor structure at a level competitive with limits from the
global analysis of all other experiments. In addition, we investigate a
generalized matter potential, whose overall scale and flavor structure are also
constrained.
Aspects of gravitational decoherence in neutrino lensing
2106.07671 [abs] [pdf]
[abstract]
by Himanshu Swami, Kinjalk Lochan, and Ketan M. Patel.
We study decoherence effects in neutrino flavour oscillations in curved
spacetime with particular emphasis on the lensing in a Schwarzschild geometry.
Assuming Gaussian wave packets for neutrinos, we argue that the decoherence
length derived from the exponential suppression of the flavour transition
amplitude depends on the proper time of the geodesic connecting the events of
the production and detection in general gravitational setting. In the weak
gravity limit, the proper time between two events of given proper distance is
smaller than that in the flat spacetime. Therefore, in presence of a
Schwarzschild object, the neutrino wave packets have to travel relatively more
physical distance in space to lapse the same amount of proper time before they
decoher. For non-radial propagation applicable to the lensing phenomena, we
show that the decoherence, in general, is sensitive to the absolute values of
neutrino masses as well as the classical trajectories taken by neutrinos
between the source and detector along with the spatial widths of neutrino wave
packets. At distances beyond the decoherence length, the probability of
neutrino flavour transition due to lensing attains a value which depends only
on the leptonic mixing parameters. Hence, the observability of neutrino lensing
significantly depends on these parameters and in-turn the lensing can provide
useful information about them.
Sterile Neutrinos
2106.05913 [abs] [pdf]
[abstract]
by Basudeb Dasgupta and Joachim Kopp.
Neutrinos, being the only fermions in the Standard Model of Particle Physics
that do not possess electromagnetic or color charges, have the unique
opportunity to communicate with fermions outside the Standard Model through
mass mixing. Such Standard Model-singlet fermions are generally referred to as
"sterile neutrinos''. In this review article, we discuss the theoretical and
experimental motivation for sterile neutrinos, as well as their
phenomenological consequences. With the benefit of hindsight in 2020, we point
out potentially viable and interesting ideas. We focus in particular on sterile
neutrinos that are light enough to participate in neutrino oscillations, but we
also comment on the benefits of introducing heavier sterile states. We discuss
the phenomenology of eV-scale sterile neutrinos in terrestrial experiments and
in cosmology, we survey the global data, and we highlight various intriguing
anomalies. We also expose the severe tension that exists between different data
sets and prevents a consistent interpretation of the global data in at least
the simplest sterile neutrino models. We discuss non-minimal scenarios that may
alleviate some of this tension. We briefly review the status of keV-scale
sterile neutrinos as dark matter and the possibility of explaining the
matter-antimatter asymmetry of the Universe through leptogenesis driven by yet
heavier sterile neutrinos.
Impact of Improved Energy Resolution on DUNE sensitivity to Neutrino
Non-Standard Interactions
2106.04597 [abs] [pdf]
[abstract]
by Sabya Sachi Chatterjee, P. S. Bhupal Dev, and Pedro A. N. Machado.
The full physics potential of the next-generation Deep Underground Neutrino
Experiment (DUNE) is still being explored. In particular, there have been some
recent studies on the possibility of improving DUNE's neutrino energy
reconstruction. The main motivation is that a better determination of the
neutrino energy in an event-by-event basis will translate into an improved
measurement of the Dirac $CP$ phase and other neutrino oscillation parameters.
To further motivate studies and improvements on the neutrino energy
reconstruction, we evaluate the impact of energy resolution at DUNE on an
illustrative new physics scenario, viz. non-standard interactions (NSI) of
neutrinos with matter. We show that a better energy resolution in comparison to
the ones given in the DUNE conceptual and technical design reports may
significantly enhance the experimental sensitivity to NSI, particularly when
degeneracies are present. While a better reconstruction of the first
oscillation peak helps disentangling standard $CP$ effects from those coming
from NSIs, we find that the second oscillation peak also plays a nontrivial
role in improving DUNE's sensitivity.
Closing the Neutrino "BSM Gap": Physics Potential of Atmospheric
Through-Going Muons at DUNE
2106.01508 [abs] [pdf]
[abstract]
by Austin Schneider, [and 3 more]Barbara Skrzypek, Carlos A. Argüelles, and Janet M. Conrad [hide authors].
Many Beyond-Standard Model physics signatures are enhanced in high-energy
neutrino interactions. To explore these signatures, ultra-large Cherenkov
detectors such as IceCube exploit event samples with charged current muon
neutrino interactions > 1 TeV. Most of these interactions occur below the
detector volume, and produce muons that enter the detector. However, the large
spacing between detectors leads to inefficiency for measuring muons with
energies below or near the critical energy of 400 GeV. In response, IceCube has
built a densely instrumented region within the larger detector. This provides
large samples of well-reconstructed interactions that are contained within the
densely instrumented region, extending up to energies of ~50 GeV. This leaves a
gap of relatively unexplored atmospheric-neutrino events with energies between
50 GeV and 1 TeV in the ultra-large detectors. In this paper we point out that
interesting Beyond Standard Model signatures may appear in this energy window,
and that early running of the DUNE far detectors can give insight into new
physics that may appear in this range.
May 2021
New sources of leptonic CP violation at the DUNE neutrino experiment
2106.00030 [abs] [pdf]
[abstract]
by A. Giarnetti and D. Meloni.
We check the capability of the DUNE neutrino experiment to detect new sources
of leptonic CP violation beside the single phase expected in the Standard
Model. We illustrate our strategy based on the measurement of CP asymmetries in
the case New Physics will show up as Non-Standard neutrino Interactions and
sterile neutrino states and show that the most promising one, once the
experimental errors are taken into account in both scenarios, is the one
related to the $\nu_\mu \to \nu_e$ transition.
Neutrino Oscillations at JUNO, the Born Rule, and Sorkin's Triple Path
Interference
2105.14061 [abs] [pdf]
[abstract]
by Patrick Huber, [and 4 more]Hisakazu Minakata, Djordje Minic, Rebekah Pestes, and Tatsu Takeuchi [hide authors].
We argue that neutrino oscillations at JUNO offer a unique opportunity to
study Sorkin's triple-path interference, which is predicted to be zero in
canonical quantum mechanics by virtue of the Born rule. In particular, we
compute the expected bounds on triple-path interference at JUNO and demonstrate
that they are comparable to those already available from electromagnetic
probes. Furthermore, the neutrino probe of the Born rule is much more direct
due to an intrinsic independence from any boundary conditions, whereas such
dependence on boundary conditions is always present in the case of
electromagnetic probes. Thus, neutrino oscillations present an ideal probe of
this aspect of the foundations of quantum mechanics.
The framework for a common origin of $δ_{\rm CKM}$ and $δ_{\rm
PMNS}$
2105.14054 [abs] [pdf]
[abstract]
by João M. Alves, [and 4 more]Francisco J. Botella, Gustavo C. Branco, Fernando Cornet-Gomez, and Miguel Nebot [hide authors].
We analyse a possible connection between CP violations in the quark and
lepton sectors, parametrised by the CKM and PMNS phases. If one assumes that CP
breaking arises from complex Yukawa couplings, both in the quark and lepton
sectors, the above connection is not possible in general, since Yukawa
couplings in the two sectors have independent flavour structures. We show that
both the CKM and PMNS phases can instead be generated by a vacuum phase in a
class of two Higgs doublet models, and in this case a connection may be
established. This scenario requires the presence of scalar FCNC at tree level,
both in the quark and lepton sectors. The appearance of these FCNC is an
obstacle and a blessing. An obstacle since one has to analyse which models are
able to conform to the strict experimental limits on FCNC, both in the quark
and lepton sectors. A blessing, because this class of models is falsifiable
since FCNC arise at a level which can be probed experimentally in the near
future, specially in the processes $h\to e^\pm\tau^\mp$ and $t\to h c$. The
connection between CP violations in CKM and PMNS is explicitely illustrated in
models with Minimal Flavour Violation.
First Dark Matter Search Results From Coherent CAPTAIN-Mills
2105.14020 [abs] [pdf]
[abstract]
by A. A. Aguilar-Arevalo, [and 49 more]S. Biedron, J. Boissevain, M. Borrego, M. Chavez-Estrada, A. Chavez, J. M. Conrad, R. L. Cooper, A. Diaz, J. R. Distel, J. D'Olivo, E. Dunton, B. Dutta, A. Elliott, D. Evans, D. Fields, J. Greenwood, M. Gold, J. Gordon, E. D. Guarincerri, E. C. Huang, N. Kamp, C. Kelsey, K. Knickerbocker, R. Lake, W. C. Louis, R. Mahapatra, S. Maludze, J. Mirabal, R. Moreno, H. Neog, P. deNiverville, V. Pandey, J. Plata-Salas, D. Poulson, H. Ray, E. Renner, T. J. Schaub, M. H. Shaevitz, D. Smith, W. Sondheim, A. M. Szelc, C. Taylor, W. H. Thompson, M. Tripathi, R. T. Thornton, R. Van Berg, R. G. Van de Water, S. Verma, and K. Walker [hide authors].
This paper describes the operation of the Coherent CAPTAIN-Mills (CCM)
detector located at the Lujan Neutron Science Center (LANSCE) at Los Alamos
National Laboratory (LANL). CCM is a 10-ton liquid argon (LAr) detector located
20 meters from a high flux neutron/neutrino source and is designed to search
for sterile neutrinos ($\nu_s$) and light dark matter (LDM). An engineering run
was performed in Fall 2019 to study the characteristics of the CCM120 detector
by searching for coherent scattering signals consistent with $\nu_s$'s and LDM
resulting from $\pi^+$ and $\pi^0$ decays in the tungsten target. New parameter
space in a leptophobic dark matter model was excluded for DM masses between
$\sim2.0$ and 30 MeV. The lessons learned from this run have guided the
development and construction of the new CCM200 detector that will begin
operations in 2021 and significantly improve on these searches.
Hot spots in the neutrino flux created by cosmic rays from Cygnus and
Vela?
2105.13378 [abs] [pdf]
[abstract]
by M. Bouyahiaoui, M. Kachelriess, and D. V. Semikoz.
An analysis of 7.5 years of data in the high-energy starting event sample has
been recently published by the IceCube collaboration. The hottest spot in a
search for neutrino sources was found far above the Galactic plane and is thus,
at first sight, difficult to reconcile with a Galactic origin. In this work, we
calculate the cosmic ray (CR) density around nearby, young supernova remnants
assuming anisotropic diffusion. Combining the obtained CR densities with the
matter distribution deduced from extinction maps, we find two prominent hot
spots: The one close to the most significant point in the IceCube search for
point sources is created by CRs from the Cygnus loop and has an intensity
corresponding to two to four neutrino events. Another, more extended one may be
caused by CRs from Vela if CR trajectories are sufficiently disturbed by the
magnetic field in the shell around the superbubble Loop I.
SN1987A still shining: A Quest for Pseudo-Dirac Neutrinos
2105.12736 [abs] [pdf]
[abstract]
by Ivan Martinez-Soler, Yuber F. Perez-Gonzalez, and Manibrata Sen.
Ever since the discovery of neutrinos, we have wondered if neutrinos are
their own antiparticles. One remarkable possibility is that neutrinos have a
pseudo-Dirac nature, predicting a tiny mass difference between active and
sterile states. We analyze the neutrino data from SN1987A in the light of
active-sterile oscillations and find a mild preference ($\Delta\chi^2\approx
3$) for $\delta m^2=6.31\times 10^{-20}{\rm eV}^2$. Notably, the same data is
able to exclude $\delta m^2\sim[2.55,3.01]\times 10^{-20}{\rm eV}^2$ with
$\Delta\chi^2> 9$, the tiniest mass differences constrained so far. We further
consider the next-generation of experiments and demonstrate their sensitivity
exploring the nature of the neutrino mass.
Probing the Particle Spectrum of Nature with Evaporating Black Holes
2105.10506 [abs] [pdf]
[abstract]
by Michael J. Baker and Andrea Thamm.
Photons radiated from an evaporating black hole in principle provide complete
information on the particle spectrum of nature up to the Planck scale. If an
evaporating black hole were to be observed, it would open a unique window onto
models beyond the Standard Model of particle physics. To demonstrate this, we
compute the limits that could be placed on the size of a dark sector. We find
that observation of an evaporating black hole at a distance of 0.01 parsecs
could probe dark sector models containing one or more copies of the Standard
Model particles, with any mass scale up to 100 TeV.
Constraining active-sterile neutrino transition magnetic moments at DUNE
near and far detectors
2105.09699 [abs] [pdf]
[abstract]
by Thomas Schwetz, Albert Zhou, and Jing-Yu Zhu.
We consider the sensitivity of the DUNE experiment to a heavy neutral lepton,
HNL (also known as sterile neutrino) in the mass range from a few MeV to a few
GeV, interacting with the Standard Model via a transition magnetic moment to
the active neutrinos, the so-called dipole portal. The HNL is produced via the
upscattering of active neutrinos, and the subsequent decay inside the detector
provides a single-photon signal. We show that the tau-neutrino dipole portal
can be efficiently probed at the DUNE far detector, using the tau-neutrino flux
generated by neutrino oscillations, while the near detector provides better
sensitivity to the electron- and muon-neutrino dipole portal. DUNE will be able
to explore large regions of currently unconstrained parameter space and has
comparable sensitivity to other planned dedicated experiments, such as SHiP. We
also comment briefly on the sensitivity to pure HNL mixing with the tau
neutrino at the DUNE far detector.
Heavy Neutrino searches through Double-Bang Events at Super-Kamiokande,
DUNE, and Hyper-Kamiokande
2105.09357 [abs] [pdf]
[abstract]
by Mack Atkinson, [and 4 more]Pilar Coloma, Ivan Martinez-Soler, Noemi Rocco, and Ian M. Shoemaker [hide authors].
A variety of new physics scenarios allow for neutrinos to up-scatter into a
heavy neutral lepton state. For a range of couplings and neutrino energies, the
heavy neutrino may travel some distance before decaying to visible final
states. When both the up-scattering and decay occur within the detector volume,
these "double bang" events produce distinctive phenomenology with very low
background. In this work, we first consider the current sensitivity at
Super-Kamiokande via the atmospheric neutrino flux, and find current data may
already provide new constraints. We then examine projected future sensitivity
at DUNE and Hyper-Kamiokande, including both atmospheric and beam flux
contributions to double-bang signals.
New Interference Effects from Light Gauge Bosons in Neutrino-Electron
Scattering
2105.09309 [abs] [pdf]
[abstract]
by P. S. Bhupal Dev, [and 3 more]Doojin Kim, Kuver Sinha, and Yongchao Zhang [hide authors].
We point out that light gauge boson mediators could induce new interference
effects in neutrino-electron scattering that can be used to enhance the
sensitivity of neutrino-flavor-selective high-intensity neutrino experiments,
such as DUNE. We particularly emphasize a destructive interference effect,
leading to a deficit between the Standard Model expectation and the
experimental measurement of the differential cross-sections, which is prominent
only in either the neutrino or the antineutrino mode, depending on the mediator
couplings. Therefore, the individual neutrino (or antineutrino) mode could
allow for sensitivity reaches superior to the combined analysis, and moreover,
could distinguish between different types of gauge boson mediators.
Violation of Equivalence Principle in Neutrino Sector: Probing the
Extended Parameter Space
2105.08744 [abs] [pdf]
[abstract]
by Arman Esmaili.
The oscillation of neutrino flavors, due to its interferometry nature, is
extremely sensitive to the phase differences developing during the propagation
of neutrinos. In this paper we investigate the effect of the Violation of
Equivalence Principle (VEP) on the flavor oscillation probabilities of
atmospheric and cosmic neutrinos observed at neutrino telescopes such as
IceCube. Assuming a general parameterization of VEP, dubbed extended parameter
space, we show that the synergy between the collected data of high energy
atmospheric and cosmic neutrinos severely constrains the VEP parameters. Also,
the projected sensitivity of IceCube-Gen2 to VEP parameters is discussed.
First direct neutrino-mass measurement with sub-eV sensitivity
2105.08533 [abs] [pdf]
[abstract]
by M. Aker, [and 127 more]A. Beglarian, J. Behrens, A. Berlev, U. Besserer, B. Bieringer, F. Block, B. Bornschein, L. Bornschein, M. Böttcher, T. Brunst, T. S. Caldwell, R. M. D. Carney, L. La Cascio, S. Chilingaryan, W. Choi, K. Debowski, M. Deffert, M. Descher, D. Díaz Barrero, P. J. Doe, O. Dragoun, G. Drexlin, K. Eitel, E. Ellinger, R. Engel, S. Enomoto, A. Felden, J. A. Formaggio, F. M. Fränkle, G. B. Franklin, F. Friedel, A. Fulst, K. Gauda, W. Gil, F. Glück, R. Grössle, R. Gumbsheimer, V. Gupta, T. Höhn, V. Hannen, N. Haußmann, K. Helbing, S. Hickford, R. Hiller, D. Hillesheimer, D. Hinz, T. Houdy, A. Huber, A. Jansen, C. Karl, F. Kellerer, J. Kellerer, M. Klein, C. Köhler, L. Köllenberger, A. Kopmann, M. Korzeczek, A. Kovalík, B. Krasch, H. Krause, N. Kunka, T. Lasserre, T. L. Le, O. Lebeda, B. Lehnert, A. Lokhov, M. Machatschek, E. Malcherek, M. Mark, A. Marsteller, E. L. Martin, C. Melzer, A. Menshikov, S. Mertens, J. Mostafa, K. Müller, S. Niemes, P. Oelpmann, D. S. Parno, A. W. P. Poon, J. M. L. Poyato, F. Priester, M. Röllig, C. Röttele, R. G. H. Robertson, W. Rodejohann, C. Rodenbeck, M. Ryšavý, R. Sack, A. Saenz, P. Schäfer, A. Schaller, L. Schimpf, K. Schlösser, M. Schlösser, L. Schlüter, S. Schneidewind, M. Schrank, B. Schulz, A. Schwemmer, M. Šefčík, V. Sibille, D. Siegmann, M. Slezák, M. Steidl, M. Sturm, M. Sun, D. Tcherniakhovski, H. H. Telle, L. A. Thorne, T. Thümmler, N. Titov, I. Tkachev, K. Urban, K. Valerius, D. Vénos, A. P. Vizcaya Hernández, C. Weinheimer, S. Welte, J. Wendel, J. F. Wilkerson, J. Wolf, S. Wüstling, W. Xu, Y. -R. Yen, S. Zadoroghny, and G. Zeller [hide authors].
We report the results of the second measurement campaign of the Karlsruhe
Tritium Neutrino (KATRIN) experiment. KATRIN probes the effective electron
anti-neutrino mass, $m_{\nu}$, via a high-precision measurement of the tritium
$\beta$-decay spectrum close to its endpoint at $18.6\,\mathrm{keV}$. In the
second physics run presented here, the source activity was increased by a
factor of 3.8 and the background was reduced by $25\,\%$ with respect to the
first campaign. A sensitivity on $m_{\nu}$ of $0.7\,\mathrm{eV/c^2}$ at
$90\,\%$ confidence level (CL) was reached. This is the first sub-eV
sensitivity from a direct neutrino-mass experiment. The best fit to the
spectral data yields $m_{\nu}^2 = (0.26\pm0.34)\,\mathrm{eV^4/c^4}$, resulting
in an upper limit of $m_{\nu}<0.9\,\mathrm{eV/c^2}$ ($90\,\%$ CL). By combining
this result with the first neutrino mass campaign, we find an upper limit of
$m_{\nu}<0.8\,\mathrm{eV/c^2}$ ($90\,\%$ CL).
Cosmological radiation density with non-standard neutrino-electron
interactions
2105.08168 [abs] [pdf]
[abstract]
by Pablo F. de Salas, [and 4 more]Stefano Gariazzo, Pablo Martínez-Miravé, Sergio Pastor, and Mariam Tórtola [hide authors].
Neutrino non-standard interactions (NSI) with electrons are known to alter
the picture of neutrino decoupling from the cosmic plasma. NSI modify both
flavour oscillations through matter effects, and the annihilation and
scattering between neutrinos and electrons and positrons in the thermal plasma.
In view of the forthcoming cosmological observations, we perform a precision
study of the impact of non-universal and flavour-changing NSI on the effective
number of neutrinos, $N_{eff}$. We present the variation of $N_{eff}$ arising
from the different NSI parameters and discuss the existing degeneracies among
them, from cosmology alone and in relation to the current bounds from
terrestrial experiments. Even though cosmology is generally less sensitive to
NSI than these experiments, we find that future cosmological data would provide
competitive and complementary constraints for some of the couplings and their
combinations.
Neutrinos as a probe of the Universe
2105.07502 [abs] [pdf]
[abstract]
by Luis A. Anchordoqui and Thomas J. Weiler.
A brief essay on how studying neutrinos can help us to better understand the
Universe.
Z-Boson Decays into Majorana or Dirac (Heavy) Neutrinos
2105.06576 [abs] [pdf]
[abstract]
by Alain Blondel, André de Gouvêa, and Boris Kayser.
We computed the kinematics of Z-boson decay into a heavy-light neutrino pair
when the Z-boson is produced at rest in electron-positron collisions, including
the subsequent decay of the heavy neutrino into a visible final state
containing a charged-lepton. We concentrated on heavy-neutrino masses of order
dozens of GeV and the issue of addressing the nature of the neutrinos - Dirac
fermions or Majorana fermions. We find that while it is not possible to tell
the nature of the heavy and light neutrinos on an event-by-event basis, the
nature of the neutrinos can nonetheless be inferred given a large-enough sample
of heavy-light neutrino pairs. We identify two observables sensitive to the
nature of neutrinos. One is the forward-backward asymmetry of the
daughter-charged-leptons. This asymmetry is exactly zero if the neutrinos are
Majorana fermions and is non-zero (and opposite) for positively- and
negatively-charged daughter-leptons if the neutrinos are Dirac fermions. The
other observable is the polarization of the heavy neutrino, imprinted in the
laboratory-frame energy distribution of the daughter-charged-leptons. Dirac
neutrinos and antineutrinos produced in electron-positron collisions at the
Z-pole are strongly polarized while Majorana neutrinos are at most as polarized
as the $Z$-bosons.
Global constraints on neutral-current generalized neutrino interactions
2105.06484 [abs] [pdf]
[abstract]
by F. J. Escrihuela, [and 3 more]L. J. Flores, O. G. Miranda, and Javier Rendón [hide authors].
We study generalized neutrino interactions (GNI) for several neutrino
processes, including neutrinos from electron-positron collisions,
neutrino-electron scattering, and neutrino deep inelastic scattering. We
constrain scalar, pseudoscalar, and tensor new physics effective couplings,
based on the standard model effective field theory at low energies. We have
performed a global analysis for the different effective couplings. We also
present the different individual constraints for each effective parameter
(scalar, pseudoscalar, and tensor). Being a global analysis, we show robust
results for the restrictions on the different GNI parameters and improve some
of these bounds.
Searching for new physics through neutrino non-standard interactions
2105.06191 [abs] [pdf]
[abstract]
by Yong Du.
Due to the absence of any definite signals of new physics at colliders and
from precision measurements, it has gradually become more and more popular in
the community to utilize the effective field theory (EFT) framework in
searching for new physics in a model-independent manner. In this letter,
working in the EFT framework and focusing on neutrino non-standard interactions
(NSIs), we report our most recent results on these NSIs from considering
terrestrial neutrino oscillation experiments Daya Bay, Double Chooz, RENO, T2K
and NO$\nu$A, and precision measurements of $N_{\rm eff}$ from Planck and
CMB-S4.
How to Assess the Carbon Footprint of a Large-Scale Physics Project
2105.04610 [abs] [pdf]
[abstract]
by Clarisse Aujoux, Odile Blanchard, and Kumiko Kotera.
Large-scale experiments are building blocks of the physics community: they
involve a large fraction of the scientific staff working in multiple countries,
and absorb a significant volume of the science budget. They are also a
collection of carbon-emitting sources and practices. As such, it is essential
to assess their environmental impact. We describe here a methodology to
estimate the main greenhouse gas (GHG) emissions of a large-scale astrophysics
collaboration project, using transparent open data. The goal is neither to
consider all possible emission sources of a project, nor to calculate accurate
values. It is rather to identify the biggest emission sources of the project,
obtain orders of magnitude for them and analyse their relative weights. We
discuss methods to quantify the GHG-generating activities and their related
emission factors for the three typical biggest emission sources that can be
controlled by the collaboration: travel, digital and hardware.
On the Tau flavor of the cosmic neutrino flux
2105.03272 [abs] [pdf]
[abstract]
by Yasaman Farzan.
Observation of high energy cosmic neutrinos by ICECUBE has ushered in a new
era in exploring both cosmos and new physics beyond the Standard Model (SM). In
the standard picture, although mostly $\nu_\mu$ and $\nu_e$ are produced in the
source, oscillation will produce $\nu_\tau$ {\it en route}. Certain beyond SM
scenarios, like interaction with ultralight DM can alter this picture. Thus,
the flavor composition of the cosmic neutrino flux can open up the possibility
of exploring certain beyond the SM scenarios that are inaccessible otherwise.
We show that the $\tau$ flavor holds a special place among the neutrino flavors
in elucidating new physics. Interpreting the two anomalous events observed by
ANITA as $\nu_\tau$ events makes the tau flavor even more intriguing. We study
how the detection of the two tau events by ICECUBE constrains the interaction
of the neutrinos with ultralight dark matter and discuss the implications of
this interaction for even higher energy cosmic neutrinos detectable by future
radio telescopes such as ARA, ARIANNA and GRAND. We also revisit the $3+1$
neutrino scheme as a solution to the two anomalous ANITA events and clarify a
misconception that exists in the literature about the evolution of high energy
neutrinos in matter within the $3+1$ scheme with a possibility of scattering
off nuclei. We show that the existing bounds on the flux of $\nu_\tau$ with
energy of EeV rules out this solution for the ANITA events. We show that the
$3+1$ solution can be saved from both this bound and from the bound on the
extra relativistic degrees of freedom in the early universe by turning on the
interaction of neutrinos with ultralight dark matter.
Dirac CP phases in a 3+1 neutrino scenario with $μ-τ$ symmetry
2105.01205 [abs] [pdf]
[abstract]
by Eduardo Becerra-García and Abdel Pérez-Lorenzana.
A sterile neutrino in the $3+1$ scheme, where the sterile accounts for
neutrino anomalies not explained solely by the weak active neutrinos, arises as
a natural source for the breaking of the $\mu-\tau$ symmetry suggested by
oscillation neutrino data. We explore the predictions for the Dirac CP phases
in this scenario, with and without sterile neutrino decay, and show that
current limits on $\delta_{CP}$ suggest a normal hierarchy and a lightest
neutrino scale below 0.1~eV as the most plausible explanation for that, when
Majorana phases are null. Other Dirac phases turn out to be non zero as well.
April 2021
High-energy cosmic neutrinos as a probe of the vector mediator scenario
in light of the muon $g-2$ anomaly and Hubble tension
2104.15136 [abs] [pdf]
[abstract]
by Jose Alonso Carpio, [and 3 more]Kohta Murase, Ian M. Shoemaker, and Zahra Tabrizi [hide authors].
In light of the recent Muon $g-2$ experiment data from Fermilab, we
investigate the implications of a gauged $L_{\mu} - L_{\tau}$ model for high
energy neutrino telescopes. It has been suggested that a new gauge boson at the
MeV scale can both account for the Muon $g-2$ data and alleviate the tension in
the Hubble parameter measurements. It also strikes signals at IceCube from the
predicted resonance scattering between high-energy neutrinos and the cosmic
neutrino background. We revisit this model based on the latest IceCube shower
data, and perform a four-parameter fit to find a preferred region. While the
data are consistent with the absence of resonant signatures from secret
interactions, we find the preferred region consistent with the muon $g-2$
anomaly and Hubble tension. We demonstrate that future neutrino telescopes such
as IceCube-Gen2 can probe this unique parameter space, and point out that
successful measurements would infer the neutrino mass with $0.05~{\rm
eV}\lesssim \Sigma m_\nu\lesssim 0.3~{\rm eV}$.
Passive low-energy nuclear recoil detection with color centers
2104.13926 [abs] [pdf]
[abstract]
by Bernadette K. Cogswell, Apurva Goel, and Patrick Huber.
Crystal damage events such as tracks and point defects have been used to
record and detect radiation for a long time and recently they have been
proposed as a means for dark matter detection. Color centers can be read out
optically and we propose a scheme based on selective plane illumination
microscopy for sub-micron imaging of large volumes corresponding to kilogram
mass detectors. This class of detectors would be passive and would operate at
room temperature. We apply these concepts to the detection of reactor neutrinos
using coherent elastic neutrino nucleus scattering (CEvNS). Crystal damage
formation energies are intrinsically on the order of 25eV, resulting in
similarly low nuclear recoil thresholds. This would enable the first
observation of reactor neutrino CEvNS with detectors as small as 10g.
Additionally, a competitive search for spin-dependent dark matter scattering
down to a dark matter mass of 0.3GeV could be possible. Passive crystal
detectors might also be attractive for nuclear non-proliferation safeguards if
used to monitor reactor power and to put limits on plutonium production. The
passive nature and small footprint of the proposed detectors implies that these
might fit well within accepted reactor safeguards operations.
CNNs for enhanced background discrimination in DSNB searches in
large-scale water-Gd detectors
2104.13426 [abs] [pdf]
[abstract]
by David Maksimović, Michael Nieslony, and Michael Wurm.
Gadolinium-loading of large water Cherenkov detectors is a prime method for
the detection of the Diffuse Supernova Neutrino Background (DSNB). While the
enhanced neutron tagging capability greatly reduces single-event backgrounds,
correlated events mimicking the IBD coincidence signature remain a potentially
harmful background. Neutral-Current (NC) interactions of atmospheric neutrinos
potentially dominate the DSNB signal especially in the low-energy range of the
observation window that reaches from about 12 to 30 MeV.
The present paper investigates a novel method for the discrimination of this
background. Convolutional Neural Networks (CNNs) offer the possibility for a
direct analysis and classification of the PMT hit patterns of the prompt
events. Based on the events generated in a simplified SuperKamiokande-like
detector setup, we find that a trained CNN can maintain a signal efficiency of
96 % while reducing the residual NC background to 2 % of the original rate.
Comparing to recent predictions of the DSNB signal and measurements of the NC
background levels in Super-Kamiokande, the corresponding signal-to-background
ratio is about 4:1, providing excellent conditions for a DSNB discovery.
The Smallest Neutrino Mass Revisited
2104.09050 [abs] [pdf]
[abstract]
by Shun Zhou.
As is well known, the smallest neutrino mass turns out to be vanishing in the
minimal seesaw model, since the effective neutrino mass matrix $M^{}_\nu$ is of
rank two due to the fact that only two heavy right-handed neutrinos are
introduced. In this paper, we point out that the one-loop matching condition
for the effective dimension-five neutrino mass operator can make an important
contribution to the smallest neutrino mass. By using the available one-loop
matching condition and two-loop renormalization group equations in the
supersymmetric version of the minimal seesaw model, we explicitly calculate the
smallest neutrino mass in the case of normal neutrino mass ordering and find
$m^{}_1 \in [10^{-10}, 10^{-8}]~{\rm eV}$ at the Fermi scale $\Lambda^{}_{\rm
F} = 91.2~{\rm GeV}$, where the range of $m^{}_1$ results from the
uncertainties on the choice of the seesaw scale $\Lambda^{}_{\rm SS}$ and on
the input values of relevant parameters at $\Lambda^{}_{\rm SS}$.
Combined analysis of neutrino decoherence at reactor experiments
2104.05806 [abs] [pdf]
[abstract]
by André de Gouvêa, Valentina De Romeri, and Christoph A. Ternes.
Reactor experiments are well suited to probe the possible loss of coherence
of neutrino oscillations due to wave-packets separation. We combine data from
the short-baseline experiments Daya Bay and the Reactor Experiment for Neutrino
Oscillation (RENO) and from the long baseline reactor experiment KamLAND to
obtain the best current limit on the reactor antineutrino wave-packet width,
$\sigma > 2.1 \times 10^{-4}$ nm at 90% CL. We also find that the determination
of standard oscillation parameters is robust, i.e., it is mostly insensitive to
the presence of hypothetical decoherence effects once one combines the results
of the different reactor neutrino experiments.
Extragalactic magnetic field constraints from ultra-high-energy cosmic
rays from local galaxies
2104.05732 [abs] [pdf]
[abstract]
by Arjen van Vliet, [and 3 more]Andrea Palladino, Andrew Taylor, and Walter Winter [hide authors].
We interpret the correlation between local star-forming galaxy positions and
ultra-high-energy cosmic ray (UHECR) directions, recently detected by the
Pierre Auger Observatory (PAO), in terms of physical parameters: the local
density of sources and the magnetic fields governing the UHECR propagation. We
include a Galactic magnetic field model on top of a random extragalactic
magnetic field description to determine the level of UHECR deflections expected
from an ensemble of source positions. Besides deflections in magnetic fields,
we also take into account energy losses with background photon fields as well
as spectrum and composition measurements by the PAO. We find consistency
between the PAO anisotropy measurement and the local star-forming galaxy
density for large extragalactic magnetic field strengths with $B > 0.2 \ \rm
nG$ (for a coherence length of $1 \ \rm Mpc$) at the $5\sigma$ confidence
level. Larger source densities lead to more isotropic background and
consequently allow for weaker extragalactic magnetic fields. However, the
acceleration of UHECR by such abundant sources is more challenging to motivate.
Too large source densities and extragalactic magnetic field strengths, on the
other hand, are also disfavored as that decreases the expected level of
anisotropy. This leads to upper limits of $B < 22 \ \rm nG$ and $\rho_0 < 8.4
\cdot 10^{-2} \ \rm Mpc^{-3}$ at the 90\% confidence level.
Three-Body Decays of Heavy Dirac and Majorana Fermions
2104.05719 [abs] [pdf]
[abstract]
by André de Gouvêa, [and 3 more]Patrick J. Fox, Boris J. Kayser, and Kevin J. Kelly [hide authors].
Nonzero neutrino masses imply the existence of degrees of freedom and
interactions beyond those in the Standard Model. A powerful indicator of what
these might be is the nature of the massive neutrinos: Dirac fermions versus
Majorana fermions. While addressing the nature of neutrinos is often associated
with searches for lepton-number violation, there are several other features
that distinguish Majorana from Dirac fermions. Here, we compute in great detail
the kinematics of the daughters of the decays into charged-leptons and
neutrinos of hypothetical heavy neutral leptons at rest. We allow for the decay
to be mediated by the most general four-fermion interaction Lagrangian. We
demonstrate, for example, that when the daughter charged-leptons have the same
flavor or the detector is insensitive to their charges, polarized
Majorana-fermion decays have zero forward/backward asymmetry in the direction
of the outgoing neutrino (relative to the parent spin), whereas Dirac-fermion
decays can have large asymmetries. Going beyond studying forward/backward
asymmetries, we also explore the fully-differential width of the three-body
decays. It contains a wealth of information not only about the nature of the
new fermions but also the nature of the interactions behind their decays.
Probing non-unitary neutrino mixing via long-baseline neutrino
oscillation experiments based at J-PARC
2104.04315 [abs] [pdf]
[abstract]
by C Soumya.
This paper investigates the capability of long-baseline experiments, which
are making use of neutrinos that are coming from Japan Proton Accelerator
Research Complex (J-PARC), in establishing the unitarity of active-neutrino
mixing by ruling out the non-unitary mixing scheme as a function of true values
of CP-violating phase $\delta_{\mathrm{CP}}$. It is found that T2HK can
establish unitarity of active neutrino mixing at above 2$\sigma$ C.L.
irrespective of neutrino mass hierarchy and true value of $\delta_{CP}$, if
non-unitary (NU) parameter $\alpha_{21}$ is of the order of $10^{-2}$. Further,
this paper is also discuss the bound on NU parameter in 21 sector and
sensitivity limit of these experiments in determining NU parameter. It is found
that the bounds on $\left(\alpha_{21}/2\right)$ are 0.028, 0.0026, 0.005 at
2$\sigma$ C.L. respectively for T2K, T2HK, and T2HKK. Moreover, it is also
found that the sensitivity limit of T2HK on NU parameter is far better than
that of both T2HKK and T2K.
Coherent neutrino scattering and the Migdal effect on the quenching
factor
2104.01811 [abs] [pdf]
[abstract]
by Jiajun Liao, Hongkai Liu, and Danny Marfatia.
Recent measurements of the germanium quenching factor deviate significantly
from the predictions of the standard Lindhard model for nuclear recoil energies
below a keV. This departure may be explained by the Migdal effect in neutron
scattering on germanium. We show that the Migdal effect on the quenching factor
can mimic the signal of a light Z' or light scalar mediator in coherent elastic
neutrino nucleus scattering experiments with reactor antineutrinos. It is
imperative that the quenching factor of nuclei with low recoil energy
thresholds be precisely measured close to threshold to avoid such confusion.
This will also help in experimental searches of light dark matter.
CP-Violating and Charged Current Neutrino Non-standard Interactions in
CE$ν$NS
2104.00425 [abs] [pdf]
[abstract]
by Amir N. Khan, Douglas W. McKay, and Werner Rodejohann.
Neutrino non-standard interactions (NSI) can be constrained using coherent
elastic neutrino-nucleus scattering. We discuss here two aspects in this
respect, namely the effects of (i) charged current NSI in neutrino production
and (ii) CP-violating phases associated with neutral current NSI in neutrino
detection. Effects of CP-phases require the simultaneous presence of two
different flavor-changing neutral current NSI parameters. Applying these two
scenarios to the COHERENT measurement, we derive limits on charged current NSI
and find that more data is required to compete with the existing limits.
Regarding CP-phases, we show how the limits on the NSI parameters depend
dramatically on the values of the phases. Accidentally, the same parameters
influencing coherent scattering also show up in neutrino oscillation
experiments. We find that COHERENT provides complementary constraints on the
set of NSI parameters that can explain the discrepancy in the best-fit value of
the standard CP-phase obtained by T2K and NO$\nu$A, while the significance with
which the LMA-Dark solution is ruled out can be weakened by the presence of
additional NSI parameters introduced here.
March 2021
Sterile neutrinos with non-standard interactions in $β$- and
$0νββ$-decay experiments
2104.00140 [abs] [pdf]
[abstract]
by Wouter Dekens, Jordy de Vries, and Tom Tong.
Charged currents are probed in low-energy precision $\beta$-decay experiments
and at high-energy colliders, both of which aim to measure or constrain signals
of beyond-the-Standard-Model physics. In light of future $\beta$-decay and LHC
measurements that will further explore these non-standard interactions, we
investigate what neutrinoless double-$\beta$ decay ($0\nu\beta\beta$)
experiments can tell us if a nonzero signal were to be found. Using a recently
developed effective-field-theory framework, we consider the effects that
interactions with right-handed neutrinos have on $0\nu\beta\beta$ and discuss
the range of neutrino masses that current and future $0\nu\beta\beta$
measurements can probe, assuming neutrinos are Majorana particles. For
non-standard interactions at the level suggested by recently observed hints in
$\beta$ decays, we show that next-generation $0\nu\beta\beta$ experiments can
determine the Dirac or Majorana nature of neutrinos, for sterile neutrino
masses larger than $\mathcal O(10)$ eV.
Boosted dark matter from diffuse supernova neutrinos
2104.00027 [abs] [pdf]
[abstract]
by Anirban Das and Manibrata Sen.
The XENON collaboration recently reported an excess of electron recoil events
in the low energy region with a significance of around $3.3\sigma$. An
explanation of this excess in terms of thermal dark matter seems challenging.
We propose a scenario where dark matter in the Milky Way halo gets boosted as a
result of scattering with the diffuse supernova neutrino background. This
interaction can accelerate the dark-matter to semi-relativistic velocities, and
this flux, in turn, can scatter with the electrons in the detector, thereby
providing a much better fit to the data. We identify regions in the parameter
space of dark-matter mass and interaction cross-section which satisfy the
excess. Furthermore, considering the data only hypothesis, we also impose
bounds on the dark-matter scattering cross-section, which are competitive with
bounds from other experiments.
Future searches for light sterile neutrinos at nuclear reactors
2104.00005 [abs] [pdf]
[abstract]
by Jeffrey M. Berryman, Luis A. Delgadillo, and Patrick Huber.
We study the optimization of a green-field, two-baseline reactor experiment
with respect to the sensitivity for electron antineutrino disappearance in
search of a light sterile neutrino. We consider both commercial and research
reactors and identify as key factors the distance of closest approach and
detector energy resolution. We find that a total of 5 tons of detectors
deployed at a commercial reactor with a closest approach of 25 m can probe the
mixing angle $\sin^22\theta$ down to $\sim5\times10^{-3}$ around $\Delta
m^2\sim 1$ eV$^2$. The same detector mass deployed at a research reactor can be
sensitive up to $\Delta m^2\sim20-30$ eV$^2$ assuming a closest approach of 3 m
and excellent energy resolution, such as that projected for the Taishan
Antineutrino Observatory. We also find that lithium doping of the reactor could
be effective in increasing the sensitivity for higher $\Delta m^2$ values.
Neutrino signals of lightcone fluctuations resulting from fluctuating
space-time
2103.15313 [abs] [pdf]
[abstract]
by Thomas Stuttard.
One of the most common expectations of a quantum theory of gravity is that
space-time is uncertain or fluctuating at microscopic scales, making it a
stochastic medium for particle propagation. Particles traversing this
space-time may experience fluctuations in travel times or velocities, together
referred to as lightcone fluctuations, with even very small effects potentially
accumulating into observable signals over large distances. In this work we
present a heuristic model of lightcone fluctuations and study the resulting
modifications to neutrino propagation, including neutrino decoherence and
arrival time spread. We show the expected scale of such effects due to
`natural' Planck scale physics and consider how they may be observed in
neutrino detectors, and compare the potential of neutrinos to $\gamma$-ray
astronomy. Using simulations of neutrino mass states propagating in a
fluctuating environment, we determine an analytic decoherence operator in the
framework of open quantum systems to quantitatively evaluate neutrino
decoherence resulting from lightcone fluctuations, allowing experimental
constraints on neutrino decoherence to be connected to Planck scale
fluctuations in space-time and $\gamma$-ray results.
Evolution of Neutrino Mass-Mixing Parameters in Matter with Non-Standard
Interactions
2103.13431 [abs] [pdf]
[abstract]
by Sanjib Kumar Agarwalla, [and 3 more]Sudipta Das, Mehedi Masud, and Pragyanprasu Swain [hide authors].
We explore the role of matter effect in the evolution of neutrino oscillation
parameters in the presence of lepton-flavor-conserving and
lepton-flavor-violating neutral-current non-standard interactions (NSI) of the
neutrino. We derive simple approximate analytical expressions showing the
evolution/running of mass-mixing parameters in matter with energy in the
presence of standard interactions (SI) and SI+NSI (considering both positive
and negative values of real NSI parameters). We observe that only the NSI
parameters in the (2,3) block, namely $\varepsilon_{\mu\tau}$ and $(\gamma -
\beta) \equiv (\varepsilon_{\tau\tau} - \varepsilon_{\mu\mu})$ affect the
running of $\theta_{23}$. Though all the NSI parameters influence the evolution
of $\theta_{13}$, $\varepsilon_{e\mu}$ and $\varepsilon_{e\tau}$ show a
stronger impact at the energies relevant for DUNE. $\theta_{12}$ quickly
approaches to $\sim$ $90^{\circ}$ with increasing energy in both SI and SI+NSI
cases. The change in $\Delta m^2_{21,m}$ is quite significant as compared to
$\Delta m^2_{31,m}$ both in SI and SI+NSI frameworks. Flipping the signs of the
NSI parameters alters the way in which mass-mixing parameters run with energy.
We demonstrate the utility of our approach in addressing several important
features related to neutrino oscillation such as: a) unraveling interesting
degeneracies between $\theta_{23}$ and NSI parameters, b) estimating the
resonance energy in presence of NSI when $\theta_{13}$ in matter becomes
maximal, c) figuring out the required baselines and energies to have maximal
matter effect in $\nu_{\mu}$ $\rightarrow$ $\nu_{e}$ transition in the presence
of different NSI parameters, and d) studying the impact of NSI parameters
$\varepsilon_{\mu\tau}$ and $(\gamma - \beta)$ on the $\nu_{\mu} \to \nu_{\mu}$
survival probability.
Non-standard neutrino oscillations: perspective from unitarity triangles
2103.11143 [abs] [pdf]
[abstract]
by Mehedi Masud, [and 3 more]Poonam Mehta, Christoph A. Ternes, and Mariam Tortola [hide authors].
We formulate an alternative approach based on unitarity triangles to describe
neutrino oscillations in presence of non-standard interactions (NSI). Using
perturbation theory, we derive the expression for the oscillation probability
in case of NSI and cast it in terms of the three independent parameters of the
leptonic unitarity triangle (LUT). The form invariance of the probability
expression (even in presence of new physics scenario as long as the mixing
matrix is unitary) facilitates a neat geometric view of neutrino oscillations
in terms of LUT. We examine the regime of validity of perturbative expansions
in the NSI case and make comparisons with approximate expressions existing in
literature. We uncover some interesting dependencies on NSI terms while
studying the evolution of LUT parameters and the Jarlskog invariant.
Interestingly, the geometric approach based on LUT allows us to express the
oscillation probabilities for a given pair of neutrino flavours in terms of
only three (and not four) degrees of freedom which are related to the geometric
properties (sides and angles) of the triangle. Moreover, the LUT parameters are
invariant under rephasing transformations and independent of the
parameterization adopted.
Coherent elastic neutrino-nucleus scattering with the $ν$BDX-DRIFT
directional detector at next generation neutrino facilities
2103.10857 [abs] [pdf]
[abstract]
by D. Aristizabal Sierra, [and 4 more]Bhaskar Dutta, Doojin Kim, Daniel Snowden-Ifft, and Louis E. Strigari [hide authors].
We discuss various aspects of a neutrino physics program that can be carried
out with the neutrino Beam-Dump eXperiment DRIFT ($\nu$BDX-DRIFT) detector
using neutrino beams produced in next generation neutrino facilities.
$\nu$BDX-DRIFT is a directional low-pressure TPC detector suitable for
measurements of coherent elastic neutrino-nucleus scattering (CE$\nu$NS) using
a variety of gaseous target materials which include carbon disulfide, carbon
tetrafluoride and tetraethyllead, among others. The neutrino physics program
includes standard model (SM) measurements and beyond the standard model (BSM)
physics searches. Focusing on the Long Baseline Neutrino Facility (LBNF)
beamline at Fermilab, we first discuss basic features of the detector and
estimate backgrounds, including beam-induced neutron backgrounds. We then
quantify the CE$\nu$NS signal in the different target materials and study the
sensitivity of $\nu$BDX-DRIFT to measurements of the weak mixing angle and
neutron density distributions. We consider as well prospects for new physics
searches, in particular sensitivities to effective neutrino non-standard
interactions.
Coherence of oscillations in matter and supernova neutrinos
2103.10149 [abs] [pdf]
[abstract]
by Yago P. Porto-Silva and Alexei Yu. Smirnov.
We study the propagation coherence for neutrino oscillations in media with
different density profiles. For each profile, we find the dependence of the
coherence length, $L_{coh}$, on neutrino energy and address the issue of
correspondence of results in the distance and energy-momentum representations.
The key new feature in matter is existence of energy ranges with enhanced
coherence around the energies $E_0$ of "infinite coherence" at which $L_{coh}
\rightarrow \infty$. In the configuration space, the infinite coherence
corresponds to equality of the (effective) group velocities of the eigenstates.
In constant density medium, there is a unique $E_0$, which coincides with the
MSW resonance energy of oscillations of mass states and is close to the MSW
resonance energy of flavor states. In the case of massless neutrinos or
negligible masses in a very dense medium the coherence persists continuously.
In the adiabatic case, the infinite coherence is realized for periodic density
change. Adiabaticity violation changes the shape factors of the wave packets
(WPs) and leads to their spread. In a medium with sharp density changes
(jumps), splitting of the eigenstates occurs at crossing of each jump. We study
the increase of the coherence length in a single jump and periodic density
jumps - castle-wall (CW) profiles. For the CW profile, there are several $E_0$
corresponding to parametric resonances. We outlined applications of the results
for supernova neutrinos. In particular, we show that coherence between two
shock wave fronts leads to observable oscillation effects, and our analysis
suggests that the decoherence can be irrelevant for flavor transformations in
the central parts of collapsing stars.
Determining the Neutrino Mass Ordering and Oscillation Parameters with
KM3NeT/ORCA
2103.09885 [abs] [pdf]
[abstract]
by S. Aiello, [and 241 more]A. Albert, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Biagi, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, M. Bouwhuis, C. Bozza, H. Brânzaş, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, D. Calvo, A. Capone, V. Carretero, P. Castaldi, S. Celli, M. Chabab, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, R. Coniglione, P. Coyle, A. Creusot, A. Cruz, G. Cuttone, R. Dallier, B. De Martino, M. De Palma, M. Di Marino, I. Di Palma, A. F. Díaz, D. Diego-Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, D. Elsaesser, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, L. A. Fusco, T. Gal, A. Garcia Soto, F. Garufi, Y. Gatelet, N. Geisselbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, D. Grasso, G. Grella, D. Guderian, C. Guidi, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, J. J. Hernández-Rey, J. Hofestädt, F. Huang, W. Idrissi Ibnsalih, G. Illuminati, C. W. James, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczyński, O. Kalekin, U. F. Katz, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, M. Kreter, V. Kulikovskiy, R. Lahmann, M. Lamoureux, G. Larosa, C. Lastoria, R. Le Breton, S. Le Stum, O. Leonardi, F. Leone, E. Leonora, N. Lessing, G. Levi, M. Lincetto, M. Lindsey Clark, T. Lipreau, F. Longhitano, D. Lopez-Coto, L. Maderer, J. Mańczak, K. Mannheim, A. Margiotta, A. Marinelli, C. Markou, L. Martin, J. A. Martínez-Mora, A. Martini, F. Marzaioli, S. Mastroianni, K. W. Melis, G. Miele, P. Migliozzi, E. Migneco, P. Mijakowski, L. S. Miranda, C. M. Mollo, M. Morganti, M. Moser, A. Moussa, R. Muller, M. Musumeci, L. Nauta, S. Navas, C. A. Nicolau, B. Ó Fearraigh, M. O'Sullivan, M. Organokov, A. Orlando, J. Palacios González, G. Papalashvili, R. Papaleo, C. Pastore, A. M. Păun, G. E. Păvălaş, C. Pellegrino, M. Perrin-Terrin, V. Pestel, P. Piattelli, C. Pieterse, K. Pikounis, O. Pisanti, C. Poirè, V. Popa, T. Pradier, G. Pühlhofer, S. Pulvirenti, O. Rabyang, F. Raffaelli, N. Randazzo, S. Razzaque, D. Real, S. Reck, G. Riccobene, A. Romanov, A. Rovelli, F. Salesa Greus, D. F. E. Samtleben, A. Sánchez Losa, M. Sanguineti, A. Santangelo, D. Santonocito, P. Sapienza, J. Schnabel, M. F. Schneider, J. Schumann, H. M. Schutte, J. Seneca, I. Sgura, R. Shanidze, A. Sharma, A. Sinopoulou, B. Spisso, M. Spurio, D. Stavropoulos, S. M. Stellacci, M. Taiuti, Y. Tayalati, E. Tenllado, H. Thiersen, S. Tingay, V. Tsourapis, E. Tzamariudaki, D. Tzanetatos, V. Van Elewyck, G. Vasileiadis, F. Versari, D. Vivolo, G. de Wasseige, J. Wilms, R. Wojaczyński, E. de Wolf, T. Yousfi, S. Zavatarelli, A. Zegarelli, D. Zito, J. D. Zornoza, J. Zúñiga, and N. Zywucka [hide authors].
The next generation of water Cherenkov neutrino telescopes in the
Mediterranean Sea are under construction offshore France (KM3NeT/ORCA) and
Sicily (KM3NeT/ARCA). The KM3NeT/ORCA detector features an energy detection
threshold which allows to collect atmospheric neutrinos to study flavour
oscillation. This paper reports the KM3NeT/ORCA sensitivity to this phenomenon.
The event reconstruction, selection and classification are described. The
sensitivity to determine the neutrino mass ordering was evaluated and found to
be 4.4 $\sigma$ if the true ordering is normal and 2.3 $\sigma$ if inverted,
after three years of data taking. The precision to measure $\Delta m^2_{32}$
and $\theta_{23}$ were also estimated and found to be $85\cdot10^{-6}$ eV$^2$
and $(^{+1.9}_{-3.1})^{\circ}$ for normal neutrino mass ordering and,
$75\cdot10^{-6}$ eV$^2$ and $(^{+2.0}_{-7.0})^{\circ}$ for inverted ordering.
Finally, a unitarity test of the leptonic mixing matrix by measuring the rate
of tau neutrinos is described. Three years of data taking were found to be
sufficient to exclude $\nu_{\tau}$ and $\bar{\nu}_{\tau}$ event rate variations
larger than 20% at $3\sigma$ level.
Sailing the CE$ν$NS Seas of Non-Standard Neutrino Interactions with
the Coherent CAPTAIN Mills Experiment
2103.08401 [abs] [pdf]
[abstract]
by Ian M. Shoemaker and Eli Welch.
We study future coherent elastic neutrino-nucleus scattering (CE$\nu$NS)
modifications from a variety of possible models at the Coherent CAPTAIN Mills
(CCM) experiment at Los Alamos. We show that large regions of Non-Standard
Neutrino Interaction (NSI) parameter space will be excluded rapidly, and that
stringent new bounds on the gauge coupling in $Z'$ models will also be placed.
As a result, CCM will be able to rule out LMA-D solutions for a large class of
models with MeV-scale mediators.
Experiment Simulation Configurations Approximating DUNE TDR
2103.04797 [abs] [pdf]
[abstract]
by DUNE Collaboration, [and 973 more]B. Abi, R. Acciarri, M. A. Acero, G. Adamov, D. Adams, M. Adinolfi, Z. Ahmad, J. Ahmed, T. Alion, S. Alonso Monsalve, C. Alt, J. Anderson, C. Andreopoulos, M. P. Andrews, F. Andrianala, S. Andringa, A. Ankowski, M. Antonova, S. Antusch, A. Aranda-Fernandez, A. Ariga, L. O. Arnold, M. A. Arroyave, J. Asaadi, A. Aurisano, V. Aushev, D. Autiero, F. Azfar, H. Back, J. J. Back, C. Backhouse, P. Baesso, L. Bagby, R. Bajou, S. Balasubramanian, P. Baldi, B. Bambah, F. Barao, G. Barenboim, G. J. Barker, W. Barkhouse, C. Barnes, G. Barr, J. Barranco Monarca, N. Barros, J. L. Barrow, A. Bashyal, V. Basque, F. Bay, J. L. Bazo Alba, J. F. Beacom, E. Bechetoille, B. Behera, L. Bellantoni, G. Bellettini, V. Bellini, O. Beltramello, D. Belver, N. Benekos, F. Bento Neves, J. Berger, S. Berkman, P. Bernardini, R. M. Berner, H. Berns, S. Bertolucci, M. Betancourt, Y. Bezawada, M. Bhattacharjee, B. Bhuyan, S. Biagi, J. Bian, M. Biassoni, K. Biery, B. Bilki, M. Bishai, A. Bitadze, A. Blake, B. Blanco Siffert, F. D. M. Blaszczyk, G. C. Blazey, E. Blucher, J. Boissevain, S. Bolognesi, T. Bolton, M. Bonesini, M. Bongrand, F. Bonini, A. Booth, C. Booth, S. Bordoni, A. Borkum, T. Boschi, N. Bostan, P. Bour, S. B. Boyd, D. Boyden, J. Bracinik, D. Braga, D. Brailsford, A. Brandt, J. Bremer, C. Brew, E. Brianne, S. J. Brice, C. Brizzolari, C. Bromberg, G. Brooijmans, J. Brooke, A. Bross, G. Brunetti, N. Buchanan, H. Budd, D. Caiulo, P. Calafiura, J. Calcutt, M. Calin, S. Calvez, E. Calvo, L. Camilleri, A. Caminata, M. Campanelli, D. Caratelli, G. Carini, B. Carlus, P. Carniti, I. Caro Terrazas, H. Carranza, A. Castillo, C. Castromonte, C. Cattadori, F. Cavalier, F. Cavanna, S. Centro, G. Cerati, A. Cervelli, A. Cervera Villanueva, M. Chalifour, C. Chang, E. Chardonnet, A. Chatterjee, S. Chattopadhyay, J. Chaves, H. Chen, M. Chen, Y. Chen, D. Cherdack, C. Chi, S. Childress, A. Chiriacescu, K. Cho, S. Choubey, A. Christensen, D. Christian, G. Christodoulou, E. Church, P. Clarke, T. E. Coan, A. G. Cocco, J. A. B. Coelho, E. Conley, J. M. Conrad, M. Convery, L. Corwin, P. Cotte, L. Cremaldi, L. Cremonesi, J. I. Crespo-Anadón, E. Cristaldo, R. Cross, C. Cuesta, Y. Cui, D. Cussans, M. Dabrowski, H. da Motta, L. Da Silva Peres, C. David, Q. David, G. S. Davies, S. Davini, J. Dawson, K. De, R. M. De Almeida, P. Debbins, I. De Bonis, M. P. Decowski, A. de Gouvêa, P. C. De Holanda, I. L. De Icaza Astiz, A. Deisting, P. De Jong, A. Delbart, D. Delepine, M. Delgado, A. Dell'Acqua, P. De Lurgio, J. R. T. de Mello Neto, D. M. DeMuth, S. Dennis, C. Densham, G. Deptuch, A. De Roeck, V. De Romeri, J. J. De Vries, R. Dharmapalan, M. Dias, F. Diaz, J. S. Díaz, S. Di Domizio, L. Di Giulio, P. Ding, L. Di Noto, C. Distefano, R. Diurba, M. Diwan, Z. Djurcic, N. Dokania, M. J. Dolinski, L. Domine, D. Douglas, F. Drielsma, D. Duchesneau, K. Duffy, P. Dunne, T. Durkin, H. Duyang, O. Dvornikov, D. A. Dwyer, A. S. Dyshkant, M. Eads, D. Edmunds, J. Eisch, S. Emery, A. Ereditato, C. O. Escobar, L. Escudero Sanchez, J. J. Evans, E. Ewart, A. C. Ezeribe, K. Fahey, A. Falcone, C. Farnese, Y. Farzan, J. Felix, E. Fernandez-Martinez, P. Fernandez Menendez, F. Ferraro, L. Fields, A. Filkins, F. Filthaut, R. S. Fitzpatrick, W. Flanagan, B. Fleming, R. Flight, J. Fowler, W. Fox, J. Franc, K. Francis, D. Franco, J. Freeman, J. Freestone, J. Fried, A. Friedland, S. Fuess, I. Furic, A. P. Furmanski, A. Gago, H. Gallagher, A. Gallego-Ros, N. Gallice, V. Galymov, E. Gamberini, T. Gamble, R. Gandhi, R. Gandrajula, S. Gao, D. Garcia-Gamez, M. Á. García-Peris, S. Gardiner, D. Gastler, G. Ge, B. Gelli, A. Gendotti, S. Gent, Z. Ghorbani-Moghaddam, D. Gibin, I. Gil-Botella, C. Girerd, A. K. Giri, D. Gnani, O. Gogota, M. Gold, S. Gollapinni, K. Gollwitzer, R. A. Gomes, L. V. Gomez Bermeo, L. S. Gomez Fajardo, F. Gonnella, J. A. Gonzalez-Cuevas, M. C. Goodman, O. Goodwin, S. Goswami, C. Gotti, E. Goudzovski, C. Grace, M. Graham, E. Gramellini, R. Gran, E. Granados, A. Grant, C. Grant, D. Gratieri, P. Green, S. Green, L. Greenler, M. Greenwood, J. Greer, W. C. Griffith, M. Groh, J. Grudzinski, K. Grzelak, W. Gu, V. Guarino, R. Guenette, A. Guglielmi, B. Guo, K. K. Guthikonda, R. Gutierrez, P. Guzowski, M. M. Guzzo, S. Gwon, A. Habig, A. Hackenburg, H. Hadavand, R. Haenni, A. Hahn, J. Haigh, J. Haiston, T. Hamernik, P. Hamilton, J. Han, K. Harder, D. A. Harris, J. Hartnell, T. Hasegawa, R. Hatcher, E. Hazen, A. Heavey, K. M. Heeger, J. Heise, K. Hennessy, S. Henry, M. A. Hernandez Morquecho, K. Herner, L. Hertel, A. S. Hesam, V Hewes, A. Higuera, T. Hill, S. J. Hillier, A. Himmel, J. Hoff, C. Hohl, A. Holin, E. Hoppe, G. A. Horton-Smith, M. Hostert, A. Hourlier, B. Howard, R. Howell, J. Huang, J. Huang, J. Hugon, G. Iles, N. Ilic, A. M. Iliescu, R. Illingworth, A. Ioannisian, R. Itay, A. Izmaylov, E. James, B. Jargowsky, F. Jediny, C. Jesùs-Valls, X. Ji, L. Jiang, S. Jiménez, A. Jipa, A. Joglekar, C. Johnson, R. Johnson, B. Jones, S. Jones, C. K. Jung, T. Junk, Y. Jwa, M. Kabirnezhad, A. Kaboth, I. Kadenko, F. Kamiya, G. Karagiorgi, A. Karcher, M. Karolak, Y. Karyotakis, S. Kasai, S. P. Kasetti, L. Kashur, N. Kazaryan, E. Kearns, P. Keener, K. J. Kelly, E. Kemp, W. Ketchum, S. H. Kettell, M. Khabibullin, A. Khotjantsev, A. Khvedelidze, D. Kim, B. King, B. Kirby, M. Kirby, J. Klein, K. Koehler, L. W. Koerner, S. Kohn, P. P. Koller, M. Kordosky, T. Kosc, U. Kose, V. A. Kostelecký, K. Kothekar, F. Krennrich, I. Kreslo, Y. Kudenko, V. A. Kudryavtsev, S. Kulagin, J. Kumar, R. Kumar, C. Kuruppu, V. Kus, T. Kutter, A. Lambert, K. Lande, C. E. Lane, K. Lang, T. Langford, P. Lasorak, D. Last, C. Lastoria, A. Laundrie, A. Lawrence, I. Lazanu, R. LaZur, T. Le, J. Learned, P. LeBrun, G. Lehmann Miotto, R. Lehnert, M. A. Leigui de Oliveira, M. Leitner, M. Leyton, L. Li, S. Li, S. W. Li, T. Li, Y. Li, H. Liao, C. S. Lin, S. Lin, A. Lister, B. R. Littlejohn, J. Liu, S. Lockwitz, T. Loew, M. Lokajicek, I. Lomidze, K. Long, K. Loo, D. Lorca, T. Lord, J. M. LoSecco, W. C. Louis, K. B. Luk, X. Luo, N. Lurkin, T. Lux, V. P. Luzio, D. MacFarland, A. A. Machado, P. Machado, C. T. Macias, J. R. Macier, A. Maddalena, P. Madigan, S. Magill, K. Mahn, A. Maio, J. A. Maloney, G. Mandrioli, J. Maneira, L. Manenti, S. Manly, A. Mann, K. Manolopoulos, M. Manrique Plata, A. Marchionni, W. Marciano, D. Marfatia, C. Mariani, J. Maricic, F. Marinho, A. D. Marino, M. Marshak, C. Marshall, J. Marshall, J. Marteau, J. Martin-Albo, N. Martinez, D. A. Martinez Caicedo, S. Martynenko, K. Mason, A. Mastbaum, M. Masud, S. Matsuno, J. Matthews, C. Mauger, N. Mauri, K. Mavrokoridis, R. Mazza, A. Mazzacane, E. Mazzucato, E. McCluskey, N. McConkey, K. S. McFarland, C. McGrew, A. McNab, A. Mefodiev, P. Mehta, P. Melas, M. Mellinato, O. Mena, S. Menary, H. Mendez, A. Menegolli, G. Meng, M. D. Messier, W. Metcalf, M. Mewes, H. Meyer, T. Miao, G. Michna, T. Miedema, J. Migenda, R. Milincic, W. Miller, J. Mills, C. Milne, O. Mineev, O. G. Miranda, S. Miryala, C. S. Mishra, S. R. Mishra, A. Mislivec, D. Mladenov, I. Mocioiu, K. Moffat, N. Moggi, R. Mohanta, T. A. Mohayai, N. Mokhov, J. Molina, L. Molina Bueno, A. Montanari, C. Montanari, D. Montanari, L. M. Montano Zetina, J. Moon, M. Mooney, A. Moor, D. Moreno, B. Morgan, C. Morris, C. Mossey, E. Motuk, C. A. Moura, J. Mousseau, W. Mu, L. Mualem, J. Mueller, M. Muether, S. Mufson, F. Muheim, A. Muir, M. Mulhearn, H. Muramatsu, S. Murphy, J. Musser, J. Nachtman, S. Nagu, M. Nalbandyan, R. Nandakumar, D. Naples, S. Narita, D. Navas-Nicolás, N. Nayak, M. Nebot-Guinot, L. Necib, K. Negishi, J. K. Nelson, J. Nesbit, M. Nessi, D. Newbold, M. Newcomer, D. Newhart, R. Nichol, E. Niner, K. Nishimura, A. Norman, A. Norrick, R. Northrop, P. Novella, J. A. Nowak, M. Oberling, A. Olivares Del Campo, A. Olivier, Y. Onel, Y. Onishchuk, J. Ott, L. Pagani, S. Pakvasa, O. Palamara, S. Palestini, J. M. Paley, M. Pallavicini, C. Palomares, E. Pantic, V. Paolone, V. Papadimitriou, R. Papaleo, A. Papanestis, S. Paramesvaran, S. Parke, Z. Parsa, M. Parvu, S. Pascoli, L. Pasqualini, J. Pasternak, J. Pater, C. Patrick, L. Patrizii, R. B. Patterson, S. J. Patton, T. Patzak, A. Paudel, B. Paulos, L. Paulucci, Z. Pavlovic, G. Pawloski, D. Payne, V. Pec, S. J. M. Peeters, Y. Penichot, E. Pennacchio, A. Penzo, O. L. G. Peres, J. Perry, D. Pershey, G. Pessina, G. Petrillo, C. Petta, R. Petti, F. Piastra, L. Pickering, F. Pietropaolo, J. Pillow, J. Pinzino, R. Plunkett, R. Poling, X. Pons, N. Poonthottathil, S. Pordes, M. Potekhin, R. Potenza, B. V. K. S. Potukuchi, J. Pozimski, M. Pozzato, S. Prakash, T. Prakash, S. Prince, G. Prior, D. Pugnere, K. Qi, X. Qian, J. L. Raaf, R. Raboanary, V. Radeka, J. Rademacker, B. Radics, A. Rafique, E. Raguzin, M. Rai, M. Rajaoalisoa, I. Rakhno, H. T. Rakotondramanana, L. Rakotondravohitra, Y. A. Ramachers, R. Rameika, M. A. Ramirez Delgado, B. Ramson, A. Rappoldi, G. Raselli, P. Ratoff, S. Ravat, H. Razafinime, J. S. Real, B. Rebel, D. Redondo, M. Reggiani-Guzzo, T. Rehak, J. Reichenbacher, S. D. Reitzner, A. Renshaw, S. Rescia, F. Resnati, A. Reynolds, G. Riccobene, L. C. J. Rice, K. Rielage, Y. Rigaut, D. Rivera, L. Rochester, M. Roda, P. Rodrigues, M. J. Rodriguez Alonso, J. Rodriguez Rondon, A. J. Roeth, H. Rogers, S. Rosauro-Alcaraz, M. Rossella, J. Rout, S. Roy, A. Rubbia, C. Rubbia, B. Russell, J. Russell, D. Ruterbories, R. Saakyan, S. Sacerdoti, T. Safford, N. Sahu, P. Sala, N. Samios, M. C. Sanchez, D. A. Sanders, D. Sankey, S. Santana, M. Santos-Maldonado, N. Saoulidou, P. Sapienza, C. Sarasty, I. Sarcevic, G. Savage, V. Savinov, A. Scaramelli, A. Scarff, A. Scarpelli, T. Schaffer, H. Schellman, P. Schlabach, D. Schmitz, K. Scholberg, A. Schukraft, E. Segreto, J. Sensenig, I. Seong, A. Sergi, F. Sergiampietri, D. Sgalaberna, M. H. Shaevitz, S. Shafaq, M. Shamma, H. R. Sharma, R. Sharma, T. Shaw, C. Shepherd-Themistocleous, S. Shin, D. Shooltz, R. Shrock, L. Simard, N. Simos, J. Sinclair, G. Sinev, J. Singh, J. Singh, V. Singh, R. Sipos, F. W. Sippach, G. Sirri, A. Sitraka, K. Siyeon, D. Smargianaki, A. Smith, A. Smith, E. Smith, P. Smith, J. Smolik, M. Smy, P. Snopok, M. Soares Nunes, H. Sobel, M. Soderberg, C. J. Solano Salinas, S. Söldner-Rembold, N. Solomey, V. Solovov, W. E. Sondheim, M. Sorel, J. Soto-Oton, A. Sousa, K. Soustruznik, F. Spagliardi, M. Spanu, J. Spitz, N. J. C. Spooner, K. Spurgeon, R. Staley, M. Stancari, L. Stanco, H. M. Steiner, J. Stewart, B. Stillwell, J. Stock, F. Stocker, T. Stokes, M. Strait, T. Strauss, S. Striganov, A. Stuart, D. Summers, A. Surdo, V. Susic, L. Suter, C. M. Sutera, R. Svoboda, B. Szczerbinska, A. M. Szelc, R. Talaga, H. A. Tanaka, B. Tapia Oregui, A. Tapper, S. Tariq, E. Tatar, R. Tayloe, A. M. Teklu, M. Tenti, K. Terao, C. A. Ternes, F. Terranova, G. Testera, A. Thea, J. L. Thompson, C. Thorn, S. C. Timm, A. Tonazzo, M. Torti, M. Tortola, F. Tortorici, D. Totani, M. Toups, C. Touramanis, J. Trevor, W. H. Trzaska, Y. T. Tsai, Z. Tsamalaidze, K. V. Tsang, N. Tsverava, S. Tufanli, C. Tull, E. Tyley, M. Tzanov, M. A. Uchida, J. Urheim, T. Usher, M. R. Vagins, P. Vahle, G. A. Valdiviesso, E. Valencia, Z. Vallari, J. W. F. Valle, S. Vallecorsa, R. Van Berg, R. G. Van de Water, D. Vanegas Forero, F. Varanini, D. Vargas, G. Varner, J. Vasel, G. Vasseur, K. Vaziri, S. Ventura, A. Verdugo, S. Vergani, M. A. Vermeulen, M. Verzocchi, H. Vieira de Souza, C. Vignoli, C. Vilela, B. Viren, T. Vrba, T. Wachala, A. V. Waldron, M. Wallbank, H. Wang, J. Wang, Y. Wang, Y. Wang, K. Warburton, D. Warner, M. Wascko, D. Waters, A. Watson, P. Weatherly, A. Weber, M. Weber, H. Wei, A. Weinstein, D. Wenman, M. Wetstein, M. R. While, A. White, L. H. Whitehead, D. Whittington, M. J. Wilking, C. Wilkinson, Z. Williams, F. Wilson, R. J. Wilson, J. Wolcott, T. Wongjirad, K. Wood, L. Wood, E. Worcester, M. Worcester, C. Wret, W. Wu, W. Wu, Y. Xiao, G. Yang, T. Yang, N. Yershov, K. Yonehara, T. Young, B. Yu, J. Yu, R. Zaki, J. Zalesak, L. Zambelli, B. Zamorano, A. Zani, L. Zazueta, G. P. Zeller, J. Zennamo, K. Zeug, C. Zhang, M. Zhao, E. Zhivun, G. Zhu, E. D. Zimmerman, M. Zito, S. Zucchelli, J. Zuklin, V. Zutshi, and R. Zwaska [hide authors].
The Deep Underground Neutrino Experiment (DUNE) is a next-generation
long-baseline neutrino oscillation experiment consisting of a high-power,
broadband neutrino beam, a highly capable near detector located on site at
Fermilab, in Batavia, Illinois, and a massive liquid argon time projection
chamber (LArTPC) far detector located at the 4850L of Sanford Underground
Research Facility in Lead, South Dakota. The long-baseline physics sensitivity
calculations presented in the DUNE Physics TDR, and in a related physics paper,
rely upon simulation of the neutrino beam line, simulation of neutrino
interactions in the near and far detectors, fully automated event
reconstruction and neutrino classification, and detailed implementation of
systematic uncertainties. The purpose of this posting is to provide a
simplified summary of the simulations that went into this analysis to the
community, in order to facilitate phenomenological studies of long-baseline
oscillation at DUNE. Simulated neutrino flux files and a GLoBES configuration
describing the far detector reconstruction and selection performance are
included as ancillary files to this posting. A simple analysis using these
configurations in GLoBES produces sensitivity that is similar, but not
identical, to the official DUNE sensitivity. DUNE welcomes those interested in
performing phenomenological work as members of the collaboration, but also
recognizes the benefit of making these configurations readily available to the
wider community.
Non-unitary neutrino mixing in short and long-baseline experiments
2103.01998 [abs] [pdf]
[abstract]
by D. V. Forero, [and 3 more]C. Giunti, C. A. Ternes, and M. Tortola [hide authors].
Non-unitary neutrino mixing in the light neutrino sector is a direct
consequence of type-I seesaw neutrino mass models. In these models, light
neutrino mixing is described by a sub-matrix of the full lepton mixing matrix
and, then, it is not unitary in general. In consequence, neutrino oscillations
are characterized by additional parameters, including new sources of CP
violation. Here we perform a combined analysis of short and long-baseline
neutrino oscillation data in this extended mixing scenario. We did not find a
significant deviation from unitary mixing, and the complementary data sets have
been used to constrain the non-unitarity parameters. We have also found that
the T2K and NOvA tension in the determination of the Dirac CP-phase is not
alleviated in the context of non-unitary neutrino mixing.
Does inhomogeneous big bang nucleosynthesis produce an inhomogeneous
element distribution today?
2103.01832 [abs] [pdf]
[abstract]
by Robert J. Scherrer.
Inhomogeneous big bang nucleosynthesis (BBN) produces a spatially
inhomogeneous distribution of element abundances at $T \sim 10^9$ K, but
subsequent element diffusion will tend to erase these inhomogeneities. We
calculate the cosmological comoving diffusion length for the BBN elements. This
diffusion length is limited by atomic scattering and is therefore dominated by
diffusion when the atoms are neutral, between the redshifts of recombination
and reionization. We find that the comoving diffusion length today is $d_{com}
\approx 70$ pc for all of the elements of interest except $^7$Li, for which
$d_{com}$ is an order of magnitude smaller because $^7$Li remains ionized
throughout the relevant epoch. This comoving diffusion length corresponds to a
substellar baryonic mass scale and is roughly equal to the horizon scale at
BBN. These results lend support to the possibility that inhomogeneities on
scales larger than the horizon at BBN could lead to a spatially inhomogeneous
distribution of elements today, while purely subhorizon fluctuations at BBN can
result only in a homogeneous element distribution at present.
Long-lived bi$\boldsymbolν$o at the LHC
2103.01251 [abs] [pdf]
[abstract]
by Julia Gehrlein and Seyda Ipek.
We examine the detection prospects for a long-lived bi$\nu$o, a pseudo-Dirac
bino which is responsible for neutrino masses, at the LHC and at dedicated
long-lived particle detectors. The bi$\nu$o arises in $U(1)_R$-symmetric
supersymmetric models where the neutrino masses are generated through higher
dimensional operators in an inverse seesaw mechanism. At the LHC the bi$\nu$o
is produced through squark decays and it subsequently decays to quarks, charged
leptons and missing energy via its mixing with the Standard Model neutrinos. We
consider long-lived bi$\nu$os which escape the ATLAS or CMS detectors as
missing energy and decay to charged leptons inside the proposed long-lived
particle detectors FASER, CODEX-b, and MATHUSLA. We find the currently allowed
region in the squark-bi$\nu$o mass parameter space by recasting most recent LHC
searches for jets+MET. We also determine the reach of MATHUSLA, CODEX-b and
FASER. We find that a large region of parameter space involving squark masses,
bi$\nu$o mass and the messenger scale can be probed with MATHUSLA, ranging from
bi$\nu$o masses of 10 GeV-2 TeV and messenger scales $10^{2-11}$ TeV for a
range of squark masses.
Robust Limits from Upcoming Neutrino Telescopes and Implications on
Minimal Dark Matter Models
2103.01237 [abs] [pdf]
[abstract]
by S. Basegmez du Pree, [and 5 more]C. Arina, A. Cheek, A. Dekker, M. Chianese, and S. Ando [hide authors].
Experimental developments in neutrino telescopes are drastically improving
their ability to constrain the annihilation cross-section of dark matter. In
this paper, we employ an angular power spectrum analysis method to probe the
galactic and extra-galactic dark matter signals with neutrino telescopes. We
first derive projections for a next generation of neutrino telescope that is
inspired by KM3NeT. We emphasise that such analysis is much less sensitive to
the choice of dark matter density profile. Remarkably, the projected
sensitivity is improved by more than an order of magnitude with respect to the
existing limits obtained by assuming the Burkert dark matter density profile
describing the galactic halo. Second, we analyse minimal extensions to the
Standard Model that will be maximally probed by the next generation of neutrino
telescopes. As benchmark scenarios, we consider Dirac dark matter in $s$- and
$t$-channel models with vector and scalar mediators. We follow a global
approach by examining all relevant complementary experimental constraints. We
find that neutrino telescopes will be able to competitively probe significant
portions of parameter space. Interestingly, the anomaly-free $L_{\mu}-L_{\tau}$
model can potentially be explored in regions where the relic abundance is
achieved through freeze-out mechanism.
Annual modulation results from three-year exposure of ANAIS-112
2103.01175 [abs] [pdf]
[abstract]
by J. Amare, [and 12 more]S. Cebrian, D. Cintas, I. Coarasa, E. Garcia, M. Martinez, M. A. Olivan, Y. Ortigoza, A. Ortiz de Solorzano, J. Puimedon, A. Salinas, M. L. Sarsa, and P. Villar [hide authors].
ANAIS (Annual modulation with NaI Scintillators) is a dark matter direct
detection experiment consisting of 112.5 kg of NaI(Tl) detectors in operation
at the Canfranc Underground Laboratory (LSC), in Spain, since August 2017.
ANAIS' goal is to confirm or refute in a model independent way the DAMA/LIBRA
positive result: an annual modulation in the low-energy detection rate having
all the features expected for the signal induced by dark matter particles in a
standard galactic halo. This modulation, observed for about 20 years, is in
strong tension with the negative results of other very sensitive experiments,
but a model-independent comparison is still lacking. By using the same target
material, NaI(Tl), such comparison is more direct and almost independent on
dark matter particle and halo models. Here, we present the annual modulation
analysis corresponding to three years of ANAIS data (for an effective exposure
of 313.95 kg$\times$y), applying a blind procedure which updates that developed
for the 1.5 years analysis, and later applied to 2 years. The analysis also
improves the background modelling in the fitting of the region of interest
rates. We obtain for the best fit in the [1-6] keV ([2-6] keV) energy region a
modulation amplitude of -0.0034$\pm$0.0042 cpd/kg/keV (0.0003$\pm$0.0037
cpd/kg/keV), supporting the absence of modulation in our data, and incompatible
with DAMA/LIBRA result at 3.3 (2.6) $\sigma$, for a sensitivity of 2.5 (2.7)
$\sigma$. Moreover, we include two complementary analyses: a phase-free annual
modulation search and the exploration of the possible presence of a periodic
signal at other frequencies. Finally, we carry out several consistency checks
of our result, and we update the ANAIS-112 projected sensitivity for the
scheduled 5 years of operation.
High Energy Neutrinos from Choked Gamma-Ray Bursts in AGN Accretion
Disks
2103.00789 [abs] [pdf]
[abstract]
by Jin-Ping Zhu, [and 5 more]Kai Wang, Bing Zhang, Yuan-Pei Yang, Yun-Wei Yu, and He Gao [hide authors].
Both long-duration gamma-ray bursts (LGRBs) from core collapse of massive
stars and short-duration GRBs (SGRBs) from mergers of binary neutron star (BNS)
or neutron star--black hole (NSBH) are expected to occur in the accretion disk
of active galactic nuclei (AGNs). We show that GRB jets embedded in the
migration traps of AGN disks are promised to be choked by the dense disk
material. Efficient shock acceleration of cosmic rays at the reverse shock is
expected, and high-energy neutrinos would be produced. We find that these
sources can effectively produce detectable TeV--PeV neutrinos through $p\gamma$
interactions. From a choked LGRB jet with isotropic equivalent energy of
$10^{53}\,{\rm erg}$ at $100\,{\rm Mpc}$, one expects $\sim2\,(7)$ neutrino
events detectable by IceCube (IceCube-Gen2). The contribution from choked LGRBs
to the observed diffuse neutrino background depends on the unknown local event
rate density of these GRBs in AGN disks. For example, if the local event rate
density of choked LGRBs in AGN disk is $\sim5\%$ that of low-luminosity GRBs
$(\sim10\,{\rm Gpc}^{-3}\,{\rm yr}^{-1})$, the neutrinos from these events
would contribute to $\sim10\%$ of the observed diffuse neutrino background.
Choked SGRBs in AGN disks are potential sources for future joint
electromagnetic, neutrino, and gravitational wave multi-messenger observations.
February 2021
LEvEL: Low-Energy Neutrino Experiment at the LHC
2103.00009 [abs] [pdf]
[abstract]
by Kevin J. Kelly, [and 3 more]Pedro A. N. Machado, Alberto Marchionni, and Yuber F. Perez-Gonzalez [hide authors].
We propose the operation of \textbf{LEvEL}, the Low-Energy Neutrino
Experiment at the LHC, a neutrino detector near the Large Hadron Collider Beam
Dump. Such a detector is capable of exploring an intense, low-energy neutrino
flux and can measure neutrino cross sections that have previously never been
observed. These cross sections can inform other future neutrino experiments,
such as those aiming to observe neutrinos from supernovae, allowing such
measurements to accomplish their fundamental physics goals. We perform detailed
simulations to determine neutrino production at the LHC beam dump, as well as
neutron and muon backgrounds. Measurements at a few to ten percent precision of
neutrino-argon charged current and neutrino-nucleus coherent scattering cross
sections are attainable with 100~ton-year and 1~ton-year exposures at LEvEL,
respectively, concurrent with the operation of the High Luminosity LHC. We also
estimate signal and backgrounds for an experiment exploiting the forward
direction of the LHC beam dump, which could measure neutrinos above 100 GeV.
Reconstruction of the neutrino mass as a function of redshift
2102.13618 [abs] [pdf]
[abstract]
by Christiane S. Lorenz, [and 3 more]Lena Funcke, Matthias Löffler, and Erminia Calabrese [hide authors].
We reconstruct the neutrino mass as a function of redshift, z, from current
cosmological data using both standard binned priors and linear spline priors
with variable knots. Using cosmic microwave background temperature,
polarization and lensing data, in combination with distance measurements from
baryonic acoustic oscillations and supernovae, we find that the neutrino mass
is consistent with $\sum m_\nu(z)$ = const. We obtain a larger bound on the
neutrino mass at low redshifts coinciding with the onset of dark energy
domination, $\sum m_\nu(z = 0)$ < 1.46 eV (95% CL). This result can be
explained either by the well-known degeneracy between $\sum m_\nu$ and
$\Omega_\Lambda$ at low redshifts, or by models in which neutrino masses are
generated very late in the Universe. We finally convert our results into
cosmological limits for models with non-relativistic neutrino decay and find
$\sum m_\nu$ < 0.21 eV (95% CL), which would be out of reach for the KATRIN
experiment.
High-Energy Neutrinos from NGC 1068
2102.12409 [abs] [pdf]
[abstract]
by Luis A. Anchordoqui, John F. Krizmanic, and Floyd W. Stecker.
IceCube has observed an excess of neutrino events over expectations from the
isotropic background from the direction of NGC 1068. The excess is inconsistent
with background expectations at the level of $2.9\sigma$ after accounting for
statistical trials. Even though the excess is not statistical significant yet,
it is interesting to entertain the possibility that it corresponds to a real
signal. Assuming a single power-law spectrum, the IceCube Collaboration has
reported a best-fit flux $\phi_\nu\sim 3 \times 10^{-8} (E_\nu/{\rm
TeV})^{-3.2}~({\rm GeV \, cm^2 \, s})^{-1}$, where $E_\nu$ is the neutrino
energy. Taking account of new physics and astronomy developments we give a
revised high-energy neutrino flux for the Stecker-Done-Salamon-Sommers AGN core
model and show that it can accommodate IceCube observations.
Resolving the LMA-dark NSI degeneracy with coherent neutrino-nucleus
scattering
2102.11981 [abs] [pdf]
[abstract]
by Mariano Esteves Chaves and Thomas Schwetz.
In the presence of non-standard neutrino interactions (NSI), a degeneracy
exists in neutrino oscillation data, which involves the flipping of the octant
of the mixing angle ${\theta_{12}}$ and the type of the neutrino mass ordering.
In this article, we revisit the status of this degeneracy in the light of
recent data on coherent elastic neutrino-nucleus scattering (CE${\nu}$NS) from
the COHERENT experiment. For general relative couplings to up and down quarks,
the degeneracy is disfavoured at the $2{\sigma}$ level by the latest data but
remains at a higher confidence level. We investigate the requirements of future
CE${\nu}$NS measurements to resolve the degeneracy with high significance. We
find that a measurement involving both, electron and muon neutrino flavours and
a target with a neutron-to-proton ratio close to 1 is required. For example, an
experiment with a silicon target at the European Spallation Source can resolve
the degeneracy at more than $4{\sigma}$ for arbitrary relative couplings to up
and down quarks.
Searching for Physics Beyond the Standard Model in an Off-Axis DUNE Near
Detector
2102.03383 [abs] [pdf]
[abstract]
by Moritz Breitbach, [and 4 more]Luca Buonocore, Claudia Frugiuele, Joachim Kopp, and Lukas Mittnacht [hide authors].
Next generation neutrino oscillation experiments like DUNE and T2HK are
multi-purpose observatories, with a rich physics program beyond oscillation
measurements. A special role is played by their near detector facilities, which
are particularly well-suited to search for weakly coupled dark sector particles
produced in the primary target. In this paper, we demonstrate this by
estimating the sensitivity of the DUNE near detectors to the scattering of
sub-GeV DM particles and to the decay of sub-GeV sterile neutrinos ("heavy
neutral leptons"). We discuss in particular the importance of the DUNE-PRISM
design, which allows some of the near detectors to be moved away from the beam
axis. At such off-axis locations, the signal-to-background ratio improves for
many new physics searches. We find that this leads to a dramatic boost in the
sensitivity to boosted DM particles interacting mainly with hadrons, while for
boosted DM interacting with leptons, data taken on-axis leads to marginally
stronger exclusion limits. Searches for heavy neutral leptons perform equally
well in both configurations.
Measuring solar neutrinos over Gigayear timescales with Paleo Detectors
2102.01755 [abs] [pdf]
[abstract]
by Natalia Tapia Arellano and Shunsaku Horiuchi.
Measuring the solar neutrino flux over gigayear timescales could provide a
new window to inform the Solar Standard Model as well as studies of the Earth's
long-term climate. We demonstrate the feasibility of measuring the
time-evolution of the $^8$B solar neutrino flux over gigayear timescales using
paleo detectors, naturally occurring minerals which record neutrino-induced
recoil tracks over geological times. We explore suitable minerals and identify
track lengths of 15--30 nm to be a practical window to detect the $^8$B solar
neutrino flux. A collection of ultra-radiopure minerals of different ages, each
some 0.1 kg by mass, can be used to probe the rise of the $^8$B solar neutrino
flux over the recent gigayear of the Sun's evolution. We also show that models
of the solar abundance problem can be distinguished based on the
time-integrated tracks induced by the $^8$B solar neutrino flux.
Exploring the Origin of Supermassive Black Holes with Coherent Neutrino
Scattering
2102.00885 [abs] [pdf]
[abstract]
by Victor Munoz, [and 3 more]Volodymyr Takhistov, Samuel J. Witte, and George M. Fuller [hide authors].
Collapsing supermassive stars ($M \gtrsim 3 \times 10^4 M_{\odot}$) at high
redshifts can naturally provide seeds and explain the origin of the
supermassive black holes observed in the centers of nearly all galaxies. During
the collapse of supermassive stars, a burst of non-thermal neutrinos is
generated with a luminosity that could greatly exceed that of a conventional
core collapse supernova explosion. In this work, we investigate the extent to
which the neutrinos produced in these explosions can be observed via coherent
elastic neutrino-nucleus scattering (CE$\nu$NS). Large scale direct dark matter
detection experiments provide particularly favorable targets. We find that
upcoming $\mathcal{O}(100)$ tonne-scale experiments will be sensitive to the
collapse of individual supermassive stars at distances as large as
$\mathcal{O}(10)$ Mpc.
January 2021
Cosmic-Neutrino-Boosted Dark Matter ($ν$BDM)
2101.11262 [abs] [pdf]
[abstract]
by Yongsoo Jho, [and 3 more]Jong-Chul Park, Seong Chan Park, and Po-Yan Tseng [hide authors].
A novel mechanism of boosting dark matter by cosmic neutrinos is proposed.
The new mechanism is so significant that the arriving flux of dark matter in
the mass window $1~{\rm keV} \lesssim m_{\rm DM} \lesssim 1~{\rm MeV}$ on Earth
can be enhanced by two to four orders of magnitude compared to one only by
cosmic electrons. Thereby we firstly derive conservative but still stringent
bounds and future sensitivity limits for such cosmic-neutrino-boosted dark
matter ($\nu$BDM) from advanced underground experiments such as Borexino,
PandaX, XENON1T, and JUNO.
Neutrino non-standard interactions meet precision measurements of
$N_{\rm eff}$
2101.10475 [abs] [pdf]
[abstract]
by Yong Du and Jiang-Hao Yu.
The number of relativistic species, $N_{\rm eff}$, has been precisely
calculated in the standard model, and would be measured to the percent level by
CMB-S4 in future. Neutral-current non-standard interactions would affect
neutrino decoupling in the early Universe, thus modifying $N_{\rm eff}$. We
parameterize those operators up to dimension-7 in the effective field theory
framework, and then provide a complete, generic and analytical dictionary for
the collision term integrals. From precision measurements of $N_{\rm eff}$, the
most stringent constraint is obtained for the dimension-6 vector-type
neutrino-electron operator, whose scale is constrained to be above about 195
(331) GeV from Planck (CMB-S4). We find our results complementary to other
experiments like neutrino coherent scattering, neutrino oscillation, collider,
and neutrino deep inelastic scattering experiments.
IceCube Data for Neutrino Point-Source Searches Years 2008-2018
2101.09836 [abs] [pdf]
[abstract]
by IceCube Collaboration, [and 373 more]R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, V. Basu, V. Baum, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, C. Bohm, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Bourbeau, F. Bradascio, J. Braun, S. Bron, J. Brostean-Kaiser, A. Burgman, J. Buscher, R. S. Busse, M. A. Campana, T. Carver, C. Chen, E. Cheung, D. Chirkin, S. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, P. Dave, C. De Clercq, J. J. DeLaunay, H. Dembinski, K. Deoskar, S. De Ridder, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, S. Dharani, A. Diaz, J. C. Díaz-Vélez, H. Dujmovic, M. Dunkman, M. A. DuVernois, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, P. A. Evenson, S. Fahey, A. R. Fazely, J. Felde, A. T. Fienberg, K. Filimonov, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, T. K. Gaisser, J. Gallagher, E. Ganster, S. Garrappa, L. Gerhardt, A. Ghadimi, T. Glauch, T. Glüsenkamp, A. Goldschmidt, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, Z. Griffith, S. Griswold, M. Gündüz, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, M. Ha Minh, K. Hanson, J. Hardin, A. Haungs, S. Hauser, D. Hebecker, P. Heix, K. Helbing, R. Hellauer, F. Henningsen, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, T. Hoinka, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, B. J. P. Jones, F. Jonske, R. Joppe, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, J. Kim, K. Kin, T. Kintscher, J. Kiryluk, T. Kittler, S. R. Klein, R. Koirala, H. Kolanoski, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, K. Krings, G. Krückl, N. Kulacz, N. Kurahashi, A. Kyriacou, C. Lagunas Gualda, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, K. Leonard, A. Leszczyńska, Y. Li, Q. R. Liu, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, J. Lünemann, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, G. Maggi, K. B. M. Mahn, Y. Makino, P. Mallik, S. Mancina, I. C. Mariş, R. Maruyama, K. Mase, R. Maunu, F. McNally, K. Meagher, A. Medina, M. Meier, S. Meighen-Berger, J. Merz, J. Micallef, D. Mockler, G. Momenté, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, P. Muth, R. Naab, R. Nagai, U. Naumann, J. Necker, G. Neer, L. V. Nguyên, H. Niederhausen, M. U. Nisa, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, M. Oehler, A. Olivas, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, P. Peiffer, C. Pérez de los Heros, S. Philippen, D. Pieloth, S. Pieper, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, P. B. Price, G. T. Przybylski, C. Raab, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, A. Rehman, R. Reimann, M. Renschler, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Scharf, M. Schaufel, H. Schieler, P. Schlunder, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, S. Sclafani, D. Seckel, S. Seunarine, S. Shefali, M. Silva, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, M. Song, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, R. G. Stokstad, N. L. Strotjohann, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, F. Tenholt, S. Ter-Antonyan, S. Tilav, K. Tollefson, L. Tomankova, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, C. F. Turley, J. P. Twagirayezu, B. Ty, E. Unger, M. A. Unland Elorrieta, J. Vandenbroucke, D. van Eijk, N. van Eijndhoven, D. Vannerom, J. van Santen, S. Verpoest, M. Vraeghe, C. Walck, A. Wallace, T. B. Watson, C. Weaver, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, B. J. Whelan, N. Whitehorn, K. Wiebe, C. H. Wiebusch, D. R. Williams, M. Wolf, T. R. Wood, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, Y. Xu, J. P. Yanez, S. Yoshida, T. Yuan, Z. Zhang, and M. Zöcklein [hide authors].
IceCube has performed several all-sky searches for point-like neutrino
sources using track-like events, including a recent time-integrated analysis
using 10 years of IceCube data. This paper accompanies the public data release
of these neutrino candidates detected by IceCube between April 6, 2008 and July
8, 2018. The selection includes through-going tracks, primarily due to muon
neutrino candidates, that reach the detector from all directions, as well as
neutrino track events that start within the instrumented volume. An updated
selection and reconstruction for data taken after April 2012 slightly improves
the sensitivity of the sample. While more than 80% of the sample overlaps
between the old and new versions, differing events can lead to changes relative
to the previous 7 year event selection. An a posteriori estimate of the
significance of the 2014-2015 TXS flare is reported with an explanation of
observed discrepancies with previous results. This public data release, which
includes 10 years of data and binned detector response functions for muon
neutrino signal events, shows improved sensitivity in generic time-integrated
point source analyses and should be preferred over previous releases.
Oscillations of sterile neutrinos from dark matter decay eliminates the
IceCube-Fermi tension
2101.09559 [abs] [pdf]
[abstract]
by Luis A. Anchordoqui, [and 4 more]Vernon Barger, Danny Marfatia, Mary Hall Reno, and Thomas J. Weiler [hide authors].
IceCube has observed a flux of cosmic neutrinos, with a "bump" in the energy
range $10 \lesssim E/{\rm TeV} \lesssim 100$ that creates a $3\sigma$ tension
with gamma-ray data from the Fermi satellite. This has been interpreted as
evidence for a population of hidden cosmic-ray accelerators. We propose an
alternative explanation of this conundrum on the basis of cold dark matter
which decays into sterile neutrinos that after oscillations produce the bump in
the cosmic neutrino spectrum.
Physics reach of a low threshold scintillating argon bubble chamber in
coherent elastic neutrino-nucleus scattering reactor experiments
2101.08785 [abs] [pdf]
[abstract]
by L. J. Flores, [and 33 more]Eduardo Peinado, E. Alfonso-Pita, K. Allen, M. Baker, E. Behnke, M. Bressler, K. Clark, R. Coppejans, C. Cripe, M. Crisler, C. E. Dahl, A. de St. Croix, D. Durnford, P. Giampa, O. Harris, P. Hatch, H. Hawley, C. M. Jackson, Y. Ko, C. Krauss, N. Lamb, M. Laurin, I. Levine, W. H. Lippincott, R. Neilson, S. Pal, M. -C. Piro, Z. Sheng, E. Vázquez-Jáuregui, T. J. Whitis, S. Windle, R. Zhang, and A. Zuñiga-Reyes [hide authors].
The physics reach of a low threshold (100 eV) scintillating argon bubble
chamber sensitive to Coherent Elastic neutrino-Nucleus Scattering (CE$\nu$NS)
from reactor neutrinos is studied. The sensitivity to the weak mixing angle,
neutrino magnetic moment, and a light $Z'$ gauge boson mediator are analyzed. A
Monte Carlo simulation of the backgrounds is performed to assess their
contribution to the signal. The analysis shows that world-leading sensitivities
are achieved with a one-year exposure for a 10 kg chamber at 3 m from a 1
MW$_{th}$ research reactor or a 100 kg chamber at 30 m from a 2000 MW$_{th}$
power reactor. Such a detector has the potential to become the leading
technology to study CE$\nu$NS using nuclear reactors.
Ultra-high energy cosmic rays deflection by the Intergalactic Magnetic
Field
2101.07207 [abs] [pdf]
[abstract]
by Andres Aramburo Garcia, [and 5 more]Kyrylo Bondarenko, Alexey Boyarsky, Dylan Nelson, Annalisa Pillepich, and Anastasia Sokolenko [hide authors].
The origin and composition of ultra-high energy cosmic rays (UHECRs) remain a
mystery. The common lore is that UHECRs are deflected from their primary
directions by the Galactic and extragalactic magnetic fields. Here we describe
an extragalactic contribution to the deflection of UHECRs that does not depend
on the strength and orientation of the initial seed field. Using the
IllustrisTNG simulations, we show that outflow-driven magnetic bubbles created
by feedback processes during galaxy formation deflect approximately half of all
$10^{20}$ eV protons by $1^{\circ}$ or more, and up to $20$-$30^{\circ}$. This
implies that the deflection in the intergalactic medium must be taken into
account in order to identify the sources of UHECRs.
Long Range Interactions in Cosmology: Implications for Neutrinos
2101.05804 [abs] [pdf]
[abstract]
by Ivan Esteban and Jordi Salvado.
Cosmology is well suited to study the effects of long range interactions due
to the large densities in the early Universe. In this article, we explore how
the energy density and equation of state of a fermion system diverge from the
commonly assumed ideal gas form under the presence of scalar long range
interactions with a range much smaller than cosmological scales. In this
scenario, "small"-scale physics can impact our largest-scale observations. As a
benchmark, we apply the formalism to self-interacting neutrinos, performing an
analysis to present and future cosmological data. Our results show that the
current cosmological neutrino mass bound is fully avoided in the presence of a
long range interaction, opening the possibility for a laboratory neutrino mass
detection in the near future. We also demonstrate an interesting
complementarity between neutrino laboratory experiments and the future EUCLID
survey.
Supernova Model Discrimination with Hyper-Kamiokande
2101.05269 [abs] [pdf]
[abstract]
by Hyper-Kamiokande Collaboration, [and 502 more]:, K. Abe, P. Adrich, H. Aihara, R. Akutsu, I. Alekseev, A. Ali, F. Ameli, I. Anghel, L. H. V. Anthony, M. Antonova, A. Araya, Y. Asaoka, Y. Ashida, V. Aushev, F. Ballester, I. Bandac, M. Barbi, G. J. Barker, G. Barr, M. Batkiewicz-Kwasniak, M. Bellato, V. Berardi, M. Bergevin, L. Bernard, E. Bernardini, L. Berns, S. Bhadra, J. Bian, A. Blanchet, F. d. M. Blaszczyk, A. Blondel, A. Boiano, S. Bolognesi, L. Bonavera, N. Booth, S. Borjabad, T. Boschi, D. Bose, S . B. Boyd, C. Bozza, A. Bravar, D. Bravo-Berguño, C. Bronner, L. Brown, A. Bubak, A. Buchowicz, M. Buizza Avanzini, F. S. Cafagna, N. F. Calabria, J. M. Calvo-Mozota, S. Cao, S. L. Cartwright, A. Carroll, M. G. Catanesi, S. Cebriàn, M. Chabera, S. Chakraborty, C. Checchia, J. H. Choi, S. Choubey, M. Cicerchia, J. Coleman, G. Collazuol, L. Cook, G. Cowan, S. Cuen-Rochin, M. Danilov, G. Daz Lopez, E. De la Fuente, P. de Perio, G. De Rosa, T. Dealtry, C. J. Densham, A. Dergacheva, N. Deshmukh, M. M. Devi, F. Di Lodovico, P. Di Meo, I. Di Palma, T. A. Doyle, E. Drakopoulou, O. Drapier, J. Dumarchez, P. Dunne, M. Dziewiecki, L. Eklund, S. El Hedri, J. Ellis, S. Emery, A. Esmaili, R. Esteve, A. Evangelisti, M. Feely, S. Fedotov, J. Feng, P. Fernandez, E. Fernández-Martinez, P. Ferrario, B. Ferrazzi, T. Feusels, A. Finch, C. Finley, A. Fiorentini, G. Fiorillo, M. Fitton, K. Frankiewicz, M. Friend, Y. Fujii, Y. Fukuda, G. Galinski, J. Gao, C. Garde, A. Garfagnini, S. Garode, L. Gialanella, C. Giganti, J. J. Gomez-Cadenas, M. Gonin, J. González-Nuevo, A. Gorin, R. Gornea, V. Gousy-Leblanc, F. Gramegna, M. Grassi, G. Grella, M. Guigue, P. Gumplinger, D. R. Hadley, M. Harada, B. Hartfiel, M. Hartz, S. Hassani, N. C. Hastings, Y. Hayato, J. A. Hernando-Morata, V. Herrero, J. Hill, K. Hiraide, S. Hirota, A. Holin, S. Horiuchi, K. Hoshina, K. Hultqvist, F. Iacob, A. K. Ichikawa, W. Idrissi Ibnsalih, T. Iijima, M. Ikeda, M. Inomoto, K. Inoue, J. Insler, A. Ioannisian, T. Ishida, K. Ishidoshiro, H. Ishino, M. Ishitsuka, H. Ito, S. Ito, Y. Itow, K. Iwamoto, A. Izmaylov, N. Izumi, S. Izumiyama, M. Jakkapu, B. Jamieson, H. I. Jang, J. S. Jang, S. J. Jenkins, S. H. Jeon, M. Jiang, H. S. Jo, P. Jonsson, K. K. Joo, T. Kajita, H. Kakuno, J. Kameda, Y. Kano, P. Kalaczynski, D. Karlen, J. Kasperek, Y. Kataoka, A. Kato, T. Katori, N. Kazarian, E. Kearns, M. Khabibullin, A. Khotjantsev, T. Kikawa, M. Kikec, J. H. Kim, J. Y. Kim, S. B. Kim, S. Y. Kim, S. King, T. Kinoshita, J. Kisiel, A. Klekotko, T. Kobayashi, L. Koch, M. Koga, L. Koerich, N. Kolev, A. Konaka, L. L. Kormos, Y. Koshio, A. Korzenev, Y. Kotsar, K. A. Kouzakov, K. L. Kowalik, L. Kravchuk, A. P. Kryukov, Y. Kudenko, T. Kumita, R. Kurjata, T. Kutter, M. Kuze, K. Kwak, M. La Commara, L. Labarga, J. Lagoda, M. Lamers James, M. Lamoureux, M. Laveder, L. Lavitola, M. Lawe, J. G. Learned, J. Lee, R. Leitner, V. Lezaun, I. T. Lim, T. Lindner, R. P. Litchfield, K. R. Long, A. Longhin, P. Loverre, X. Lu, L. Ludovici, Y. Maekawa, L. Magaletti, K. Magar, K. Mahn, Y. Makida, M. Malek, M. Malinský, T. Marchi, L. Maret, C. Mariani, A. Marinelli, K. Martens, Ll. Marti, J. F. Martin, D. Martin, J. Marzec, T. Matsubara, R. Matsumoto, S. Matsuno, M. Matusiak, E. Mazzucato, M. McCarthy, N. McCauley, J. McElwee, C. McGrew, A. Mefodiev, A. Medhi, P. Mehta, L. Mellet, H. Menjo, P. Mermod, C. Metelko, M. Mezzetto, J. Migenda, P. Migliozzi, P. Mijakowski, S. Miki, E. W. Miller, H. Minakata, A. Minamino, S. Mine, O. Mineev, A. Mitra, M. Miura, R. Moharana, C. M. Mollo, T. Mondal, M. Mongelli, F. Monrabal, D. H. Moon, C. S. Moon, F. J. Mora, S. Moriyama, Th. A. Mueller, L. Munteanu, K. Murase, Y. Nagao, T. Nakadaira, K. Nakagiri, M. Nakahata, S. Nakai, Y. Nakajima, K. Nakamura, KI. Nakamura, H. Nakamura, Y. Nakano, T. Nakaya, S. Nakayama, K. Nakayoshi, L. Nascimento Machado, C. E. R. Naseby, B. Navarro-Garcia, M. Needham, T. Nicholls, K. Niewczas, Y. Nishimura, E. Noah, F. Nova, J. C. Nugent, H. Nunokawa, W. Obrebski, J. P. Ochoa-Ricoux, E. O'Connor, N. Ogawa, T. Ogitsu, K. Ohta, K. Okamoto, H. M. O'Keeffe, K. Okumura, Y. Onishchuk, F. Orozco-Luna, A. Oshlianskyi, N. Ospina, M. Ostrowski, E. O'Sullivan, L. O'Sullivan, T. Ovsiannikova, Y. Oyama, H. Ozaki, M. Y. Pac, P. Paganini, V. Palladino, V. Paolone, M. Pari, S. Parsa, J. Pasternak, C. Pastore, G. Pastuszak, D. A. Patel, M. Pavin, D. Payne, C. Peña-Garay, C. Pidcott, E. Pinzon Guerra, S. Playfer, B. W. Pointon, A. Popov, B. Popov, K. Porwit, M. Posiadala-Zezula, J. -M. Poutissou, J. Pozimski, G. Pronost, N. W. Prouse, P. Przewlocki, B. Quilain, A. A. Quiroga, E. Radicioni, B. Radics, P. J. Rajda, J. Renner, M. Rescigno, F. Retiere, G. Ricciardi, C. Riccio, B. Richards, E. Rondio, H. J. Rose, B. Roskovec, S. Roth, C. Rott, S. D. Rountree, A. Rubbia, A. C. Ruggeri, C. Ruggles, S. Russo, A. Rychter, D. Ryu, K. Sakashita, S. Samani, F. Sánchez, M. L. Sánchez, M. C. Sanchez, S. Sano, J. D. Santos, G. Santucci, P. Sarmah, I. Sashima, K. Sato, M. Scott, Y. Seiya, T. Sekiguchi, H. Sekiya, J. W. Seo, S. H. Seo, D. Sgalaberna, A. Shaikhiev, Z. Shan, A. Shaykina, I. Shimizu, C. D. Shin, M. Shinoki, M. Shiozawa, G. Sinnis, N. Skrobova, K. Skwarczynski, M. B. Smy, J. Sobczyk, H. W. Sobel, F. J. P. Soler, Y. Sonoda, R. Spina, B. Spisso, P. Spradlin, K. L. Stankevich, L. Stawarz, S. M. Stellacci, K. Stopa, A. I. Studenikin, S. L. Suárez Gómez, T. Suganuma, S. Suvorov, Y. Suwa, A. T. Suzuki, S. Y. Suzuki, Y. Suzuki, D. Svirida, R. Svoboda, M. Taani, M. Tada, A. Takeda, Y. Takemoto, A. Takenaka, A. Taketa, Y. Takeuchi, V. Takhistov, H. Tanaka, H. A. Tanaka, H. I. Tanaka, M. Tanaka, T. Tashiro, M. Thiesse, L. F. Thompson, J. Toledo, A. K. Tomatani-Sánchez, G. Tortone, K. M. Tsui, T. Tsukamoto, M. Tzanov, Y. Uchida, M. R. Vagins, S. Valder, V. Valentino, G. Vasseur, A. Vijayvargi, C. Vilela, W. G. S. Vinning, D. Vivolo, T. Vladisavljevic, R. B. Vogelaar, M. M. Vyalkov, T. Wachala, J. Walker, D. Wark, M. O. Wascko, R. A. Wendell, R. J. Wilkes, M. J. Wilking, J. R. Wilson, S. Wronka, J. Xia, Z. Xie, T. Xin, Y. Yamaguchi, K. Yamamoto, C. Yanagisawa, T. Yano, S. Yen, N. Yershov, D. N. Yeum, M. Yokoyama, M. Yonenaga, J. Yoo, I. Yu, M. Yu, T. Zakrzewski, B. Zaldivar, J. Zalipska, K. Zaremba, G. Zarnecki, M. Ziembicki, K. Zietara, M. Zito, and S. Zsoldos [hide authors].
Core-collapse supernovae are among the most magnificent events in the
observable universe. They produce many of the chemical elements necessary for
life to exist and their remnants -- neutron stars and black holes -- are
interesting astrophysical objects in their own right. However, despite
millennia of observations and almost a century of astrophysical study, the
explosion mechanism of core-collapse supernovae is not yet well understood.
Hyper-Kamiokande is a next-generation neutrino detector that will be able to
observe the neutrino flux from the next galactic core-collapse supernova in
unprecedented detail. We focus on the first 500 ms of the neutrino burst,
corresponding to the accretion phase, and use a newly-developed, high-precision
supernova event generator to simulate Hyper-Kamiokande's response to five
different supernova models. We show that Hyper-Kamiokande will be able to
distinguish between these models with high accuracy for a supernova at a
distance of up to 100 kpc. Once the next galactic supernova happens, this
ability will be a powerful tool for guiding simulations towards a precise
reproduction of the explosion mechanism observed in nature.
The Imprint of Large Scale Structure on the Ultra-High-Energy Cosmic Ray
Sky
2101.04564 [abs] [pdf]
[abstract]
by Chen Ding, Noemie Globus, and Glennys R. Farrar.
Ultra-high-energy cosmic rays (UHECRs) are atomic nuclei from space with
vastly higher energies than any other particles ever observed. Their origin and
chemical composition remain a mystery. As we show here, the large- and
intermediate-angular-scale anisotropies observed by the Pierre Auger
Observatory are a powerful tool for understanding the origin of UHECRs. Without
specifying any particular production mechanism, but only postulating that the
source distribution follows the matter distribution of the local Universe, a
good accounting of the magnitude, direction and energy dependence of the dipole
anisotropy at energies above $8 \times 10^{18}$ eV is obtained, after taking
into account the impact of energy losses during propagation (the "GZK
horizon"), diffusion in extragalactic magnetic field and deflections in the
Galactic magnetic field (GMF). This is a major step toward the long-standing
hope of using UHECR anisotropies to constrain UHECR composition and magnetic
fields. The observed dipole anisotropy is incompatible with a pure proton
composition in this scenario. With a more accurate treatment of energy losses,
it should be possible to further constrain the cosmic-ray composition and
properties of the extragalactic magnetic field, self-consistently improve the
GMF model, and potentially expose individual UHECR sources.
New CP Phase and Exact Oscillation Probabilities of Dirac Neutrino
derived from Relativistic Equation
2101.03555 [abs] [pdf]
[abstract]
by Keiichi Kimura and Akira Takamura.
We present a new formulation deriving the neutrino oscillation probabilities
relativistically based on not the Schr$\ddot{\rm o}$dinger equation but the
Dirac equation. In two generations, we calculate the oscillation probabilities
exactly in the case that there exists only the Dirac mass term. We find that
two kinds of new terms appear in the oscillation probabilities derived from the
Dirac equation. One is the term dependent on the absolute value of neutrino
mass. Although it has been considered that the oscillation probabilities depend
only on the mass squared differences until now, we could observe the absolute
value of mass through neutrino oscillations in principle. The other is the term
including a new CP phase. If there are some interactions to distinguish the
flavors of right-handed neutrinos beyond the Standard Model, we could also
observe this new CP phase in principle even in the framework of two
generations. We discuss the possibility to observe the contribution of these
terms by the neutrino oscillations of atomic size. On the other hand, it is
negligible in the usual short and long-baseline experiments, and there is no
contradiction with previous experiments.
A New Approach to Probe Non-Standard Interactions in Atmospheric
Neutrino Experiments
2101.02607 [abs] [pdf]
[abstract]
by Anil Kumar, [and 3 more]Amina Khatun, Sanjib Kumar Agarwalla, and Amol Dighe [hide authors].
We propose a new approach to explore the neutral-current non-standard
neutrino interactions (NSI) in atmospheric neutrino experiments using
oscillation dips and valleys in reconstructed muon observables, at a detector
like ICAL that can identify the muon charge. We focus on the flavor-changing
NSI parameter $\varepsilon_{\mu\tau}$, which has the maximum impact on the muon
survival probability in these experiments. We show that non-zero
$\varepsilon_{\mu\tau}$ shifts the oscillation dip locations in $L/E$
distributions of the up/down event ratios of reconstructed $\mu^-$ and $\mu^+$
in opposite directions. We introduce a new variable $\Delta d$ representing the
difference of dip locations in $\mu^-$ and $\mu^+$, which is sensitive to the
magnitude as well as the sign of $\varepsilon_{\mu\tau}$, and is independent of
the value of $\Delta m^2_{32}$. We further note that the oscillation valley in
the ($E$, $\cos \theta$) plane of the reconstructed muon observables bends in
the presence of NSI, its curvature having opposite signs for $\mu^-$ and
$\mu^+$. We demonstrate the identification of NSI with this curvature, which is
feasible for detectors like ICAL having excellent muon energy and direction
resolutions. We illustrate how the measurement of contrast in the curvatures of
valleys in $\mu^-$ and $\mu^+$ can be used to estimate $\varepsilon_{\mu\tau}$.
Using these proposed oscillation dip and valley measurements, the achievable
precision on $|\varepsilon_{\mu\tau}|$ at 90% C.L. is about 2% with 500
kt$\cdot$yr exposure. The effects of statistical fluctuations, systematic
errors, and uncertainties in oscillation parameters have been incorporated
using multiple sets of simulated data. Our method would provide a direct and
robust measurement of $\varepsilon_{\mu\tau}$ in the multi-GeV energy range.
Estimating the carbon footprint of the GRAND Project, a multi-decade
astrophysics experiment
2101.02049 [abs] [pdf]
[abstract]
by Clarisse Aujoux, Kumiko Kotera, and Odile Blanchard.
We present a pioneering estimate of the global yearly greenhouse gas
emissions of a large-scale Astrophysics experiment over several decades: the
Giant Array for Neutrino Detection (GRAND). The project aims at detecting
ultra-high energy neutrinos with a 200,000 radio antenna array over
200,000\,km$^2$ as of the 2030s. With a fully transparent methodology based on
open source data, we calculate the emissions related to three unavoidable
sources: travel, digital technologies and hardware equipment. We find that
these emission sources have a different impact depending on the stages of the
experiment. Digital technologies and travel prevail for the small-scale
prototyping phase (GRANDProto300), whereas hardware equipment (material
production and transportation) and data transfer/storage largely outweigh the
other emission sources in the large-scale phase (GRAND200k). In the mid-scale
phase (GRAND10k), the three sources contribute equally. This study highlights
the considerable carbon footprint of a large-scale astrophysics experiment, but
also shows that there is room for improvement. We discuss various lines of
actions that could be implemented. The GRAND project being still in its
prototyping stage, our results provide guidance to the future collaborative
practices and instrumental design in order to reduce its carbon footprint.
December 2020
What if a specific neutrinoless double beta decay is absent
2012.13186 [abs] [pdf]
[abstract]
by Takehiko Asaka, Hiroyuki Ishida, and Kazuki Tanaka.
We consider the seesaw model with two right-handed neutrinos $N_1$ and $N_2$
which masses are hierarchical, and investigate their contribution to the
neutrinoless double beta ($0 \nu \beta \beta$) decay. Although the lepton
number is broken by the Majorana masses of right-handed neutrinos, such decay
processes can be absent in some cases. We present a possibility where the
lighter $N_1$ gives a destructive contribution to that of active neutrinos by
choosing the specific mixing elements of $N_1$, while $N_2$ is sufficiently
heavy not to contribute to the $0 \nu \beta \beta$ decay. In this case the
mixing elements of $N_1$ in the charged current interaction are determined by
its mass and the Majorana phase of active neutrinos. We then study the impacts
of such a possibility on the direct search for $N_1$. In addition, we discuss
the consequence of the case when the $0 \nu \beta \beta$ decay in one specific
nucleus is absent.
Lunar neutrinos
2012.12870 [abs] [pdf]
[abstract]
by S. Demidov and D. Gorbunov.
Cosmic rays bombard the lunar surface producing mesons, which attenuate
inside the regolith. They get slower and decay weakly into mostly sub-GeV
neutrinos leaving the surface. Thus the Moon shines in neutrinos. Here we
calculate spectra of low energy neutrinos, which exhibit bright features
potentially recognisable above isotropic neutrino background in the direction
towards the Moon. Their observation, though a very challenging task for future
neutrino large volume experiments, would make the Moon the nearest
astrophysical source for which the concept of multimessenger astronomy works
truly. Remarkably, some features of the lunar neutrino flux are sensitive to
the surface mass density of the Moon.
Compact Dark Objects in Neutron Star Mergers
2012.11908 [abs] [pdf]
[abstract]
by Andreas Bauswein, [and 4 more]Gang Guo, Jr-Hua Lien, Yen-Hsun Lin, and Meng-Ru Wu [hide authors].
We estimate the long-lasting gravitational wave (GW) emission of compact dark
objects following a binary neutron-star (NS) merger. We consider compact dark
objects, which initially reside in the centers of NSs and which may consist of
self-interacting dark matter (DM). By approximating the compact dark objects as
test particles, we model the merging of NS binaries hosting DM components with
three-dimensional relativistic simulations. Our simulation results suggest that
the DM components remain gravitationally bound and orbit inside the merger
remnant with orbital separations of typically a few km. The subsequent orbital
motion of the DM components generates a GW signal with frequencies in the range
of a few kHz. When considering a range of different binary masses and
high-density equations of state (EoS), we find that the GW frequency of the
orbiting DM components scales with the compactness of NSs. Similarly, we find
relations between the DM GW frequency and the dominant postmerger GW frequency
of the stellar fluid or the tidal deformability, which quantifies EoS effects
during the binary inspiral. Hence, a measurement of these quantities can be
used to specify the frequency range of the GW emission by DM. Under the
assumption that GW back reaction is the only relevant dissipative process, the
GW signal may last between seconds and years depending on the mass of the DM
component. We estimate the detectability of the GW signals and find that DM
components in NS mergers may only be detectable with existing and projected GW
instruments if the dark objects are as massive as about 0.01 to 0.1 M_sun. We
emphasize that the GW emission is limited by the lifetime of the remnant. A
forming black hole will immediately swallow the DM objects because their orbits
are smaller than the innermost stable circular orbit of the black hole.
A closer look at the $pp$-chain reaction in the Sun: Constraining the
coupling of light mediators to protons
2012.11620 [abs] [pdf]
[abstract]
by Anna M. Suliga, Shashank Shalgar, and George M. Fuller.
The $pp$-chain of nuclear reactions is the primary route for energy
production in the Sun. The first step in that reaction sequence converts two
protons to a deuterium nucleus with the emission of a positron and electron
neutrino. This reaction is extremely slow because it is a weak interaction, and
significantly, it involves quantum tunneling through the Coulomb barrier.
Though the reaction rate can be calculated with high confidence in the Standard
Model, it has not been measured at solar energies. If there exist interactions
that are engendered by non-standard mediators then the rate of this reaction in
the Sun could be altered. We probe such non-standard interactions by comparing
calculations of solar evolution to the current solar system age in the presence
and absence of the non-standard mediators. These reveal ranges of non-standard
mediator mass and couplings that are inconsistent with measured properties of
the Sun, including solar neutrino results. Our constraints on these
non-standard parameters, in many cases overlapping those derived via other
considerations, could be extended further with better confidence in the value
of the metalicity of the Sun and the solar neutrino CNO flux. Intriguingly, our
work reveals a degeneracy between the solar metalicity and the presence of the
invoked non-standard mediators.
Physics prospects with the second oscillation maximum at Deep
Underground Neutrino Experiment
2012.08269 [abs] [pdf]
[abstract]
by Jogesh Rout, [and 3 more]Sheeba Shafaq, Mary Bishai, and Poonam Mehta [hide authors].
Current long-baseline neutrino-oscillation experiments such as NO$\nu$A and
T2K are mainly sensitive to physics in the neighbourhood of the first
oscillation maximum of the $\nu_\mu \to \nu_e$ oscillation probability. The
future Deep Underground Neutrino Experiment (DUNE) utilizes a wide-band beam
tune optimized for CP violation sensitivity that fully covers the region of the
first maxima and part of the second. In the present study, we elucidate the
role of second oscillation maximum in addressing issues pertaining to unknowns
in the standard three flavour paradigm. We consider a new DUNE beam tune
optimized for coverage of the region of the second oscillation maxima which
could be realized using proposed accelerator upgrades that provide multi-MW of
power at proton energies of 8 GeV. We find that addition of the multi-MW 8 GeV
beam to DUNE wide-band running leads to modest improvement in sensitivity to CP
violation, mass hierarchy, the octant of $\theta_{23}$ as well as the
resolution of $\delta$ and the Jarlskog invariant. Significant improvements to
the DUNE neutrino energy resolution yield a much larger improvement in
performance. We conclude that the standard DUNE wide-band beam when coupled
with excellent detector resolution capabilities is sufficient to resolve
$\delta$ to better than $\sim 12^\circ$ for all values of $\delta$ in a decade
of running. For second maxima (8 GeV 3MW) beam running concurrently with the
standard wide-band (80 GeV 2.2 MW) beam for 5 of the 10 years, it is found that
$\delta$ can be further resolved better than $\sim 10^\circ$ for all values of
$\delta$.
Evolution of perturbation and power spectrum in a two-component
ultralight axionic universe
2012.07602 [abs] [pdf]
[abstract]
by Yi-Hsiung Hsu and Tzihong Chiueh.
The evolution of cosmic perturbations in a two-component ultralight axionic
universe is investigated. We present the first spectral computation of
perturbations in multi-component universes. A particular case composed of light
extreme axions and free massive particles offers a possibility for the
formation of very high-redshift massive galaxies, which are typically required
to host massive early quasars. Our computation retains the information of
perturbed velocities for individual axion components, opening a new avenue for
setting up initial conditions for future axion dark matter simulations.
Interplay between the factorization of the Jarlskog Invariant and
location of the Solar and Atmospheric Resonances for Neutrino Oscillations in
Matter
2012.07186 [abs] [pdf]
[abstract]
by Stephen J. Parke.
The Jarlskog invariant which controls the size of intrinsic CP violation in
neutrino oscillation appearance experiments is modified by Wolfenstein matter
effects for neutrinos propagating in matter. In this paper we give the exact
factorization of Jarlskog invariant in matter into the vacuum Jarlskog
invariant times two, two-flavor matter resonance factors that control the
matter effects for the solar and atmospheric resonances independently. We
compare the location of the minima of the factorizing resonance factors with
the location of the solar and atmospheric resonances, precisely defined. They
are not identical but the fractional differences are both found to be less than
0.1\%. In addition, we explain why symmetry polynomials of the square of the
mass of the neutrino eigenvalues in matter, such as inverse of the square of
the Jarlskog invariant in matter, can be given as polynomials in the matter
potential.
Review of Atmospheric Neutrino Results from Super-Kamiokande
2012.06864 [abs] [pdf]
[abstract]
by Volodymyr Takhistov.
While neutrino physics enters precision era, several important unknowns
remain. Atmospheric neutrinos allow to simultaneously test key oscillation
parameters, with Super-Kamiokande experiment playing a central role. We discuss
results from atmospheric neutrino oscillation analysis of the full dataset from
Super-Kamiokande I-IV phases. Further, we discuss tests of non-standard
neutrino interactions with atmospheric neutrinos in Super-Kamiokande.
The spectra and composition of Ultra High Energy Cosmic Rays and the
measurement of the proton-air cross section
2012.06861 [abs] [pdf]
[abstract]
by Paolo Lipari.
The shape of the longitudinal development of the showers generated in the
atmosphere by very high energy cosmic ray particles encodes information about
the mass composition of the flux, and about the properties of hadronic
interactions that control the shower development. Studies of the energy
dependence of the average and width of the depth of maximum distribution of
showers with $E \gtrsim 10^{17.3}$ eV measured by the Pierre Auger Observatory,
suggest, on the basis of a comparison with current models, that the composition
of the cosmic ray flux undergoes a very important evolution, first becoming
lighter and then rapidly heavier. These conclusions, if confirmed, would have
profound and very surprising implications for our understanding of the high
energy astrophysical sources. Studies of the shape of the depth of maximum
distribution in the same energy range have been used by Auger and by the
Telescope Array Collaboration to measure the interaction length of protons in
air, a quantity that allows to estimate the $pp$ cross sections for values of
$\sqrt{s}$ well above the LHC range. In this paper we argue that it is
desirable to combine the studies of the cosmic ray composition with those aimed
at the measurement of the $p$--air cross section. The latter allow to obtain
estimates for the fraction of protons in the flux that can be of great help in
decoding the composition and its energy dependence. Studies that consider
multiple parameters to characterize the depth of maximum distributions also
offer the possibility to perform more sensitive tests of the validity of the
models used to describe high energy showers.
Interference and Oscillation in Nambu Quantum Mechanics
2012.06583 [abs] [pdf]
[abstract]
by Djordje Minic, Tatsu Takeuchi, and Chia Hsiung Tze.
Nambu Quantum Mechanics, proposed in Phys. Lett. B536, 305 (2002), is a
deformation of canonical Quantum Mechanics in which only the time-evolution of
the "phases" of energy eigenstates is modified. We discuss the effect this
theory will have on oscillation phenomena, and place a bound on the deformation
parameters utilizing the data on the atmospheric neutrino mixing angle
$\theta_{23}$.
Contribution of Secondary Neutrinos from Line-of-sight Cosmic Ray
Interactions to the IceCube Diffuse Astrophysical Flux
2012.05955 [abs] [pdf]
[abstract]
by Alina Kochocki, [and 3 more]Volodymyr Takhistov, Alexander Kusenko, and Nathan Whitehorn [hide authors].
In ten years of observations, the IceCube neutrino observatory has revealed a
neutrino sky in tension with previous expectations for neutrino point source
emissions. Astrophysical objects associated with hadronic processes might act
as production sites for neutrinos, observed as point sources at Earth. Instead,
a nearly isotropic flux of astrophysical neutrinos is observed up to PeV
energies, prompting a reassessment of the assumed transport and production
physics. This work applies a new physical explanation for neutrino production
from populations of active galactic nuclei (AGN) and starburst galaxies to
three years of public IceCube point source data. Specifically, cosmic rays
(CRs) produced at such sources might interact with extragalactic background
light and gas along the line of sight, generating a secondary neutrino flux.
This model is tested alongside a number of typical flux weighting schemes, in
all cases the all-sky flux contribution being constrained to percent levels of
the reported IceCube diffuse astrophysical flux.
Invisible neutrino decay : First vs second oscillation maximum
2012.04958 [abs] [pdf]
[abstract]
by Kaustav Chakraborty, [and 3 more]Debajyoti Dutta, Srubabati Goswami, and Dipyaman Pramanik [hide authors].
We study the physics potential of the long-baseline experiments T2HK, T2HKK
and ESS$\nu$SB in the context of invisible neutrino decay. We consider normal
mass ordering and assume that the state $\nu_{3}$ as unstable, decaying into
sterile states during the flight and obtain constraints on the neutrino decay
lifetime ($\tau_3$). We find that T2HK, T2HKK and ESS$\nu$SB are sensitive to
the decay-rate of $\nu_{3}$ for $\tau_{3}/m_{3} \leq 2.72\times10^{-11}$s/eV,
$\tau_{3}/m_{3} \leq 4.36\times10^{-11}$s/eV and $\tau_{3}/m_{3} \leq
2.43\times10^{-11}$s/eV respectively at 3$\sigma$ C.L. We compare and contrast
the sensitivities of the three experiments and specially investigate the role
played by the mixing angle $\theta_{23}$. It is seen that for experiments with
flux peak near the second oscillation maxima, the poorer sensitivity to
$\theta_{23}$ results in weaker constraints on the decay lifetime. Although,
T2HKK has one detector close to the second oscillation maxima, having another
detector at the first oscillation maxima results in superior sensitivity to
decay. In addition, we find a synergy between the two baselines of the T2HKK
experiment which helps in giving a better sensitivity for $\theta_{23}$ in the
higher octant. We discuss the octant sensitivity in presence of decay and show
that there is an enhancement in sensitivity which occurs due to the
contribution from the survival probability $P_{\mu\mu}$ which is more
pronounced for the experiments at the second oscillation maxima. We also obtain
the combined sensitivity of T2HK+ESS$\nu$SB and T2HKK+ESS$\nu$SB as
$\tau_{3}/m_{3} \leq 4.36\times10^{-11}$s/eV and $\tau_{3}/m_{3} \leq
5.53\times10^{-11}$s/eV respectively at 3$\sigma$ C.L.
Diophantine equations with sum of cubes and cube of sum
2012.04139 [abs] [pdf]
[abstract]
by Bogdan A. Dobrescu and Patrick J. Fox.
We solve Diophantine equations of the type $ \, a \, (x^3 + y^3 + z^3 ) = (x
+ y + z)^3$, where $x,y,z$ are integer variables, and the coefficient $a \neq
0$ is rational. We show that there are infinite families of such equations,
including those where $a$ is any ratio of cubes or certain rational fractions,
that have nontrivial solutions. There are also infinite families of equations
that do not have any nontrivial solution, including those where $1/a = 1 -
24/m$ with certain restrictions on the integer $m$. The equations can be
represented by elliptic curves unless $a = 9$ or 1. If $a$ is an integer and
two variables are equal and nonzero, there exist nontrivial solutions only for
$a=4$ or 9; there are no solutions for $a = 4$ when $xyz \neq 0$. Without
imposing constraints on the variables, we find the general solution for $a =
9$, which depends on two integer parameters. These cubic equations are
important in particle physics, because they determine the fermion charges under
the $U(1)$ gauge group.
Leptonic Sum Rules from Flavour Models with Modular Symmetries
2012.04131 [abs] [pdf]
[abstract]
by Julia Gehrlein and Martin Spinrath.
Sum rules in the lepton sector provide an extremely valuable tool to classify
flavour models in terms of relations between neutrino masses and mixing
parameters testable in a plethora of experiments. In this manuscript we
identify new leptonic sum rules arising in models with modular symmetries with
residual symmetries. These models simultaneously present neutrino mass sum
rules, involving masses and Majorana phases, and mixing sum rules, connecting
the mixing angles and the Dirac CP-violating phase. The simultaneous appearance
of both types of sum rules leads to some non-trivial interplay, for instance,
the allowed absolute neutrino mass scale exhibits a dependence on the Dirac
CP-violating phase. We derive analytical expressions for these novel sum rules
and present their allowed parameter ranges as well as their predictions at
upcoming neutrino experiments.
Search for solar electron anti-neutrinos due to spin-flavor precession
in the Sun with Super-Kamiokande-IV
2012.03807 [abs] [pdf]
[abstract]
by Super-Kamiokande Collaboration, [and 201 more]:, K. Abe, C. Bronner, Y. Hayato, M. Ikeda, S. Imaizumi, H. Ito, J. Kameda, Y. Kataoka, M. Miura, S. Moriyama, Y. Nagao, M. Nakahata, Y. Nakajima, S. Nakayama, T. Okada, K. Okamoto, A. Orii, G. Pronost, H. Sekiya, M. Shiozawa, Y. Sonoda, Y. Suzuki, A. Takeda, Y. Takemoto, A. Takenaka, H. Tanaka, T. Yano, R. Akutsu, S. Han, T. Kajita, K. Okumura, T. Tashiro, R. Wang, J. Xia, D. Bravo-Berguño, L. Labarga, Ll. Marti, B. Zaldivar, F. d. M. Blaszczyk, E. Kearns, J. L. Raaf, J. L. Stone, L. Wan, T. Wester, B. W. Pointin, J. Bian, N. J. Griskevich, W. R. Kropp, S. Locke, S. Mine, M. B. Smy, H. W. Sobel, V. Takhistov, P. Weatherly, J. Hill, J. Y. Kim, I. T. Lim, R. G. Park, B. Bodur, K. Scholberg, C. W. Walter, L. Bernard, A. Coffani, O. Drapier, S. El Hedri, A. Giampaolo, M. Gonin, Th. A. Mueller, P. Paganini, B. Quilain, T. Ishizuka, T. Nakamura, J. S. Jang, J. G. Learned, L. H. V. Anthony, A. A. Sztuc, Y. Uchida, V. Berardi, M. G. Catanesi, E. Radicioni, N. F. Calabria, L. N. Machado, G. De Rosa, G. Collazuol, F. Iacob, M. Lamoureux, N. Ospina, L. Ludovici, Y. Nishimura, S. Cao, M. Friend, T. Hasegawa, T. Ishida, M. Jakkapu, T. Kobayashi, T. Matsubara, T. Nakadaira, K. Nakamura, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, Y. Nakano, T. Shiozawa, A. T. Suzuki, Y. Takeuchi, S. Yamamoto, A. Ali, Y. Ashida, J. Feng, S. Hirota, A. K. Ichikawa, T. Kikawa, M. Mori, T. Nakaya, R. A. Wendell, Y. Yasutome, P. Fernandez, N. McCauley, P. Mehta, A. Pritchard, K. M. Tsui, Y. Fukuda, Y. Itow, H. Menjo, T. Niwa, K. Sato, M. Tsukada, P. Mijakowski, C. K. Jung, C. Vilela, M. J. Wilking, C. Yanagisawa, M. Harada, K. Hagiwara, T. Horai, H. Ishino, S. Ito, Y. Koshio, W. Ma, N. Piplani, S. Sakai, Y. Kuno, G. Barr, D. Barrow, L. Cook, A. Goldsack, S. Samani, C. Simpson, D. Wark, F. Nova, T. Boschi, F. Di Lodovico, M. Taani, J. Migenda, S. Molina Sedgwick, S. Zsoldos, J. Y. Yang, S. J. Jenkins, M. Malek, J. M. McElwee, O. Stone, M. D. Thiesse, L. F. Thompson, H. Okazawa, S. B. Kim, I. Yu, K. Nishijima, M. Koshiba, K. Iwamoto, N. Ogawa, M. Yokoyama, K. Martens, M. R. Vagins, S. Izumiyama, M. Kuze, M. Tanaka, T. Yoshida, M. Inomoto, M. Ishitsuka, R. Matsumoto, K. Ohta, M. Shinoki, J. F. Martin, H. A. Tanaka, T. Towstego, M. Hartz, A. Konaka, P. de Perio, N. W. Prouse, S. Chen, B. D. Xu, B. Richards, B. Jamieson, J. Walker, A. Minamino, K. Okamoto, G. Pintaudi, R. Sasaki, and M. Posiadala-Zezula [hide authors].
Due to a very low production rate of electron anti-neutrinos ($\bar{\nu}_e$)
via nuclear fusion in the Sun, a flux of solar $\bar{\nu}_e$ is unexpected. An
appearance of $\bar{\nu}_e$ in solar neutrino flux opens a new window for the
new physics beyond the standard model. In particular, a spin-flavor precession
process is expected to convert an electron neutrino into an electron
anti-neutrino (${\nu_e\to\bar{\nu}_e}$) when neutrino has a finite magnetic
moment. In this work, we have searched for solar $\bar{\nu}_e$ in the
Super-Kamiokande experiment, using neutron tagging to identify their inverse
beta decay signature. We identified 78 $\bar{\nu}_e$ candidates for neutrino
energies of 9.3 to 17.3 MeV in 2970.1 live days with a fiducial volume of 22.5
kiloton water (183.0 kton$\cdot$year exposure). The energy spectrum has been
consistent with background predictions and we thus derived a 90% confidence
level upper limit of ${4.7\times10^{-4}}$ on the $\nu_e\to\bar{\nu}_e$
conversion probability in the Sun. We used this result to evaluate the
sensitivity of future experiments, notably the Super-Kamiokande Gadolinium
(SK-Gd) upgrade.
Significance of Composition-Dependent Effects in Fifth-Force Searches
2012.02862 [abs] [pdf]
[abstract]
by Ephraim Fischbach, [and 5 more]John T. Gruenwald, Dennis E. Krause, Megan H. McDuffie, Michael J. Mueterthies, and Carol Y. Scarlett [hide authors].
Indications of a possible composition-dependent fifth force, based on a
reanalysis of the E\"{o}tv\"{o}s experiment, have not been supported by a
number of modern experiments. Here, we argue that searching for a
composition-dependent fifth force necessarily requires data from experiments in
which the acceleration differences of three or more independent pairs of test
samples of varying composition are determined. We suggest that a new round of
fifth-force experiments is called for, in each of which three or more different
pairs of samples are compared.
Search for Coherent Elastic Scattering of Solar $^8$B Neutrinos in the
XENON1T Dark Matter Experiment
2012.02846 [abs] [pdf]
[abstract]
by E. Aprile, [and 137 more]J. Aalbers, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, F. D. Amaro, S. Andaloro, V. C. Antochi, E. Angelino, J. R. Angevaare, F. Arneodo, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, J. M. R. Cardoso, D. Cichon, B. Cimmino, M. Clark, D. Coderre, A. P. Colijn, J. Conrad, J. Cuenca, J. P. Cussonneau, M. P. Decowski, A. Depoian, P. Di Gangi, A. Di Giovanni, R. Di Stefano, S. Diglio, A. Elykov, A. D. Ferella, W. Fulgione, P. Gaemers, R. Gaior, M. Galloway, F. Gao, L. Grandi, C. Hils, K. Hiraide, L. Hoetzsch, J. Howlett, M. Iacovacci, Y. Itow, F. Joerg, N. Kato, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, H. Landsman, R. F. Lang, L. Levinson, S. Liang, S. Lindemann, M. Lindner, F. Lombardi, J. Long, J. A. M. Lopes, Y. Ma, C. Macolino, J. Mahlstedt, A. Mancuso, L. Manenti, A. Manfredini, F. Marignetti, T. Marrodán Undagoitia, K. Martens, J. Masbou, D. Masson, S. Mastroianni, M. Messina, K. Miuchi, K. Mizukoshi, A. Molinario, K. Morå, S. Moriyama, Y. Mosbacher, M. Murra, J. Naganoma, K. Ni, U. Oberlack, K. Odgers, J. Palacio, B. Pelssers, R. Peres, M. Pierre, J. Pienaar, V. Pizzella, G. Plante, J. Qi, J. Qin, D. Ramírez García, S. Reichard, A. Rocchetti, N. Rupp, J. M. F. dos Santos, G. Sartorelli, J. Schreiner, D. Schulte, H. Schulze Eißing, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, E. Shockley, M. Silva, H. Simgen, A. Takeda, C. Therreau, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, K. Valerius, M. Vargas, G. Volta, Y. Wei, C. Weinheimer, M. Weiss, D. Wenz, C. Wittweg, T. Wolf, Z. Xu, M. Yamashita, J. Ye, G. Zavattini, Y. Zhang, T. Zhu, and J. P. Zopounidis [hide authors].
We report on a search for nuclear recoil signals from solar $^8$B neutrinos
elastically scattering off xenon nuclei in XENON1T data, lowering the energy
threshold from 2.6 keV to 1.6 keV. We develop a variety of novel techniques to
limit the resulting increase in backgrounds near the threshold. No significant
$^8$B neutrino-like excess is found in an exposure of 0.6 t $\times$ y. For the
first time, we use the non-detection of solar neutrinos to constrain the light
yield from 1-2 keV nuclear recoils in liquid xenon, as well as non-standard
neutrino-quark interactions. Finally, we improve upon world-leading constraints
on dark matter-nucleus interactions for dark matter masses between 3 GeV/c$^2$
and 11 GeV/c$^2$ by as much as an order of magnitude.
Prospects of detecting the reactor $\bar{ν_e}$-Ar coherent elastic
scattering with a low threshold dual-phase argon time projection chamber at
Taishan
2012.00966 [abs] [pdf]
[abstract]
by Yu-Ting Wei, [and 9 more]Meng-Yun Guan, Jin-Chang Liu, Ze-Yuan Yu, Chang-Gen Yang, Cong Guo, Wei-Xing Xiong, You-Yu Gan, Qin Zhao, and Jia-Jun Li [hide authors].
We propose to measure the coherent elastic neutrino nucleus scattering
(CE$\nu$NS) using a dual-phase liquid argon time projection chamber (TPC) with
200kg fiducial mass. The detector is expected to be adjacent to the JUNO-TAO
experiment and to be about 35m from a reactor core with 4.6GW thermal power at
Taishan. The antineutrino flux is approximately
6$\times10^{12}$cm$^{-1}$s$^{-1}$ at this location, leading to more than 11,000
coherent scattering events per day in the fiducial mass. However, the nuclear
recoil energies concentrate in the sub-keV region, corresponding to less than
ten ionisation electrons in the liquid argon. The detection of several
ionisation electrons can be achieved in the dual-phase TPC due to the large
amplification in the gas region. With a feasible detection threshold of four
ionisation electrons, the signal rate is 955 per day. The detector is designed
to be shielded well from cosmogenic backgrounds and ambient radioactivities to
reach a 16% background-to-signal ratio in the energy region of interest. With
the large CE$\nu$NS sample, the expected sensitivity of measuring the weak
mixing angle $\sin^{2}\theta_{W}$, and of limiting the neutrino magnetic moment
are discussed. In addition, a synergy between the reactor antineutrino
CE$\nu$NS experiment and the dark matter experiment is foreseen.
November 2020
Non-standard interactions in SMEFT confronted with terrestrial neutrino
experiments
2011.14292 [abs] [pdf]
[abstract]
by Yong Du, [and 4 more]Hao-Lin Li, Jian Tang, Sampsa Vihonen, and Jiang-Hao Yu [hide authors].
The Standard Model Effective Field Theory (SMEFT) provides a systematic and
model-independent framework to study neutrino non-standard interactions (NSIs).
We study the constraining power of the on-going neutrino oscillation
experiments T2K, NO$\nu$A, Daya Bay, Double Chooz and RENO in the SMEFT
framework. A full consideration of matching is provided between different
effective field theories and the renormalization group running at different
scales, filling the gap between the low-energy neutrino oscillation experiments
and SMEFT at the UV scale. We first illustrate our method with a top-down
approach in a simplified scalar leptoquark model, showing more stringent
constraints from the neutrino oscillation experiments compared to collider
studies. We then provide a bottom-up study on individual dimension-6 SMEFT
operators and find NSIs in neutrino experiments already sensitive to new
physics at $\sim$20 TeV when the Wilson coefficients are fixed at unity. We
also investigate the correlation among multiple operators at the UV scale and
find it could change the constraints on SMEFT operators by several orders of
magnitude compared with when only one operator is considered. Furthermore, we
find that accelerator and reactor neutrino experiments are sensitive to
different SMEFT operators, which highlights the complementarity of the two
experiment types.
Probing UHECR production in Centaurus A using secondary neutrinos and
gamma-rays
2011.13984 [abs] [pdf]
[abstract]
by Cainã de Oliveira and Vitor de Souza.
In this paper, the production of neutrinos and photons by ultra high energy
cosmic rays (UHECR) interacting with the extragalactic background radiation is
studied. Centaurus A is assumed as the prime source of UHECR and the
possibility to identify this source by detecting the secondary neutrinos and
photons produced in the propagation of UHECR is investigated. Fifteen
astrophysical models regarding three extragalactic magnetic fields (EGMF) and
five composition abundances are simulated. The flux and arrival direction of
neutrinos and photons are investigated. It is shown that the detection of a
signal from Cen A with statistical significance is achievable by current
observatories in a few years and by proposed experiments in the near future.
The dependence of the results on the models is also presented.
Flavour specific neutrino self-interaction: $H_0$ tension and IceCube
2011.13685 [abs] [pdf]
[abstract]
by Arindam Mazumdar, Subhendra Mohanty, and Priyank Parashari.
Self-interaction in the active neutrinos is studied in the literature to
alleviate the $H_0$ tension. Similar self-interaction can also explain the
observed dips in the flux of the neutrinos coming from the distant
astro-physical sources in IceCube detectors. In contrast to the flavour
universal neutrino interaction considered for solving the $H_0$ tension, which
is ruled out from particle physics experiments, we consider flavour specific
neutrino interactions. We show that the values of self-interaction coupling
constant and mediator mass required for explaining the IceCube dips are
inconsistent with the strong neutrino self-interactions preferred by the
combination of BAO, HST and Planck data. However, the required amount of
self-interaction between tau neutrinos ($\nu_\tau$) in inverted hierarchy for
explaining IceCube dips is consistent with the moderate self-interaction region
of cosmological bounds at 1-$\sigma$ level. For the case of other interactions
and hierarchies, the IceCube preferred amount of self-interaction is consistent
with moderate self-interaction region of cosmological bounds at 2-$\sigma$
level only.
UHECR mass composition at highest energies from anisotropy of their
arrival directions
2011.11590 [abs] [pdf]
[abstract]
by M. Yu. Kuznetsov and P. G. Tinyakov.
We propose a new method for the estimation of ultra-high energy cosmic ray
(UHECR) mass composition from a distribution of their arrival directions. The
method employs a test statistic (TS) based on a characteristic deflection of
UHECR events with respect to the distribution of luminous matter in the local
Universe. Making realistic simulations of the mock UHECR sets, we show that
this TS is robust to the presence of galactic and non-extreme extra-galactic
magnetic fields and sensitive to the mass composition of events in a set. This
allows one to constrain the UHECR mass composition by comparing the TS
distribution of a composition model in question with the data TS, and to
discriminate between different composition models. While the statistical power
of the method depends somewhat on the MF parameters, this dependence decreases
with the growth of statistics. The method shows good performance even at GZK
energies where the estimation of UHCER mass composition with traditional
methods is complicated by a low statistics.
Flavor Triangle of the Diffuse Supernova Neutrino Background
2011.10933 [abs] [pdf]
[abstract]
by Zahra Tabrizi and Shunsaku Horiuchi.
Although Galactic core-collapse supernovae (SNe) only happen a few times per
century, every hour a vast number of explosions happen in the whole universe,
emitting energy in the form of neutrinos, resulting in the diffuse supernova
neutrino background (DSNB). The DSNB has not yet been detected, but
Super-Kamiokande doped with gadolinium is expected to yield the first
statistically significant observation within the next several years. Since the
neutrinos produced at the core collapse undergo mixing during their propagation
to Earth, the flavor content at detection is a test of oscillation physics. In
this paper, we estimate the expected DSNB data at the DUNE, Hyper-K and JUNO
experiments which when combined are sensitive to all different neutrino
flavors. We determine how well the flavor content of the DSNB will be
reconstructed in the future, for a Mikheyev-Smirnov-Wolfenstein (MSW) scenario
as well as a neutrino decay scenario. A large fraction of the flavor space will
be excluded, but the heavy-lepton neutrino flux remains a challenge.
Novel approach for the study of coherent elastic neutrino-nucleus
scattering
2011.10230 [abs] [pdf]
[abstract]
by A. Galindo-Uribarri, O. G. Miranda, and G. Sanchez Garcia.
We propose the use of isotopically highly enriched detectors for the precise
study of coherent-elastic neutrino-nucleus scattering (CEvNS). CEvNS has been
measured for the first time in CsI and recently confirmed with a liquid argon
detector. It is expected that several new experimental setups will measure this
process with increasing accuracy. Taking Ge detectors as a working example, we
demonstrate that a combination of different isotopes is an excellent option to
do precision neutrino physics with CEvNS, test Standard Model predictions, and
probe new physics scenarios. Experiments based on this new idea can make
simultaneous differential CEvNS measurements with detectors of different
isotopic composition. Particular combination of observables could be used to
cancel systematic errors. While many applications are possible, we illustrate
the idea with three examples: testing the dominant quadratic dependence on the
number of neutrons, $N$, that is predicted by the theoretical models;
constraining the average neutron root mean square (rms) radius; and testing the
weak mixing angle and the sensitivity to new physics. In all three cases we
find that the extra sensitivity provided by this method will potentially allow
high-precision robust measurements with CEvNS and particularly, will resolve
the characteristic degeneracies appearing in new physics scenarios.
Superradiance Exclusions in the Landscape of Type IIB String Theory
2011.08693 [abs] [pdf]
[abstract]
by Viraf M. Mehta, [and 5 more]Mehmet Demirtas, Cody Long, David J. E. Marsh, Liam McAllister, and Matthew J. Stott [hide authors].
We obtain constraints from black hole superradiance in an ensemble of
compactifications of type IIB string theory. The constraints require knowing
only the axion masses and self-interactions, and are insensitive to the
cosmological model. We study more than $2 \cdot 10^5$ Calabi-Yau manifolds with
Hodge numbers $1\leq h^{1,1}\leq 491$ and compute the axion spectrum at two
reference points in moduli space for each geometry. Our computation of the
classical theory is explicit, while for the instanton-generated axion potential
we use a conservative model. The measured properties of astrophysical black
holes exclude parts of our dataset. At the point in moduli space corresponding
to the tip of the stretched K\"{a}hler cone, we exclude $\approx 50\%$ of
manifolds in our sample at 95% C.L., while further inside the K\"{a}hler cone,
at an extremal point for realising the Standard Model, we exclude a maximum of
$\approx 7\%$ of manifolds at $h^{1,1}=11$, falling to nearly zero by
$h^{1,1}=100$.
Neutrino amplitude decomposition in matter
2011.08415 [abs] [pdf]
[abstract]
by Hisakazu Minakata.
Observation of the interference between the atmospheric-scale and solar-scale
oscillations is one of the challenging and tantalizing goals of the ongoing and
upcoming neutrino experiments. An inevitable first step required for such
analyses is to establish the way of how the oscillation $S$ matrix can be
decomposed into the atmospheric and solar waves, the procedure dubbed as the
amplitude decomposition. In this paper, with use of the perturbative framework
proposed by Denton et al. (DMP), we establish the prescription for amplitude
decomposition which covers the whole kinematical region of the terrestrial
neutrino experiments. We analyze the limits to the atmospheric- and
solar-resonance regions to argue that the dynamical two modes of the DMP
decomposition can be interpreted as the matter-dressed atmospheric and solar
oscillations. The expressions of the oscillation probability, which are
decomposed into the non-interference and interference terms, are derived for
all the relevant flavor oscillation channels. Through construction of the DMP
decomposition, we reveal the nature of $\psi$ ($\theta_{12}$ in matter)
symmetry as due to the $S$ matrix rephasing invariance. A new picture of the
DMP perturbation theory emerged, a unified perturbative framework for neutrino
oscillation in earth matter.
Summary of the NuSTEC Workshop on Neutrino-Nucleus Pion Production in
the Resonance Region
2011.07166 [abs] [pdf]
[abstract]
by L. Aliaga, [and 22 more]A. Ashkenazi, C. Bronner, J. Calcutt, D. Cherdack, K. Duffy, S. Dytman, N. Jachowicz, M. Kabirnezhad, K. Kuzmin, G. A. Miller, T. Le, J. G. Morfin, U. Mosel, J. Nieves, K. Niewczas, A. Nikolakopoulos, J. Nowak, J. Paley, G. Pawloski, T. Sato, L. Weinstein, and C. Wret [hide authors].
The NuSTEC workshop held at the University of Pittsburgh in October 2019
brought theorists and experimentalists together to discuss the state of
modeling and measurements related to pion production in neutrino-nucleus
scattering in the kinematic region where pions are produced through both
resonant and non-resonant mechanisms. Modeling of this region is of critical
importance to the current and future accelerator- and atmospheric-based
neutrino oscillation experiments. For the benefit of the community, links to
the presentations are accompanied by annotations from the speakers highlighting
significant points made during the presentations and resulting discussions.
Constraints on ultralight scalar bosons within black hole spin
measurements from LIGO-Virgo's GWTC-2
2011.06010 [abs] [pdf]
[abstract]
by Ken K. Y. Ng, [and 3 more]Salvatore Vitale, Otto A. Hannuksela, and Tjonnie G. F. Li [hide authors].
Clouds of ultralight bosons - such as axions - can form around a rapidly
spinning black hole, if the black hole radius is comparable to the bosons'
wavelength. The cloud rapidly extracts angular momentum from the black hole,
and reduces it to a characteristic value that depends on the boson's mass as
well as on the black hole mass and spin. Therefore, a measurement of a black
hole mass and spin can be used to reveal or exclude the existence of such
bosons. Using the black holes released by LIGO and Virgo in their GWTC-2, we
perform a simultaneous measurement of the black hole spin distribution at
formation and the mass of the scalar boson. We find that the data strongly
disfavors the existence of scalar bosons in the mass range between
$1.3\times10^{-13}~\mathrm{eV}$ and $2.7\times10^{-13}~\mathrm{eV}$ for a decay
constant $f_a\gtrsim 10^{14}~\mathrm{GeV}$. The statistical evidence is mostly
driven by the two {binary black holes} systems GW190412 and GW190517, which
host rapidly spinning black holes. The region where bosons are excluded narrows
down if these two systems merged shortly ($\sim 10^5$ years) after the black
holes formed.
Flavor-dependent radiative corrections in coherent elastic
neutrino-nucleus scattering
2011.05960 [abs] [pdf]
[abstract]
by Oleksandr Tomalak, [and 3 more]Pedro Machado, Vishvas Pandey, and Ryan Plestid [hide authors].
We calculate coherent elastic neutrino-nucleus scattering cross sections on
spin-0 nuclei (e.g. $^{40}$Ar and $^{28}$Si) at energies below 100 MeV within
the Standard Model and account for all effects of permille size. We provide a
complete error budget including uncertainties at nuclear, nucleon, hadronic,
and quark levels separately as well as perturbative error. Our calculation
starts from the four-fermion effective field theory to explicitly separate
heavy-particle mediated corrections (which are absorbed by Wilson coefficients)
from light-particle contributions. Electrons and muons running in loops
introduce a nontrivial dependence on the momentum transfer due to their
relatively light masses. These same loops, and those mediated by tau leptons,
break the flavor universality because of mass-dependent electromagnetic
radiative corrections. Nuclear physics uncertainties significantly cancel in
flavor asymmetries resulting in subpercent relative errors. We find that for
low neutrino energies, the cross section can be predicted with a relative
precision that is competitive with neutrino-electron scattering. We highlight
potentially useful applications of such a precise cross section prediction
ranging from precision tests of the Standard Model, to searches for new physics
and to the monitoring of nuclear reactors.
First all-flavor search for transient neutrino emission using 3-years of
IceCube DeepCore data
2011.05096 [abs] [pdf]
[abstract]
by R. Abbasi, [and 362 more]M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, V. Basu, V. Baum, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Bourbeau, F. Bradascio, J. Braun, S. Bron, J. Brostean-Kaiser, A. Burgman, R. S. Busse, M. A. Campana, C. Chen, D. Chirkin, S. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, P. Dave, C. De Clercq, J. J. DeLaunay, H. Dembinski, K. Deoskar, S. De Ridder, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, S. Dharani, A. Diaz, J. C. Díaz-Vélez, H. Dujmovic, M. Dunkman, M. A. DuVernois, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, J. Evans, P. A. Evenson, S. Fahey, A. R. Fazely, S. Fiedlschuster, A. T. Fienberg, K. Filimonov, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, S. Garrappa, L. Gerhardt, A. Ghadimi, T. Glauch, T. Glüsenkamp, A. Goldschmidt, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, Z. Griffith, S. Griswold, M. Gündüz, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, M. Ha Minh, K. Hanson, J. Hardin, A. Haungs, S. Hauser, D. Hebecker, K. Helbing, F. Henningsen, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, T. Hoinka, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, B. J. P. Jones, R. Joppe, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, J. Kim, K. Kin, T. Kintscher, J. Kiryluk, S. R. Klein, R. Koirala, H. Kolanoski, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, K. Krings, G. Krückl, N. Kurahashi, A. Kyriacou, C. Lagunas Gualda, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, K. Leonard, A. Leszczyńska, Y. Li, Q. R. Liu, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, P. Mallik, S. Mancina, I. C. Mariş, R. Maruyama, K. Mase, F. McNally, K. Meagher, M. Medici, A. Medina, M. Meier, S. Meighen-Berger, J. Merz, J. Micallef, D. Mockler, G. Momenté, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, R. Naab, R. Nagai, U. Naumann, J. Necker, G. Neer, L. V. Nguyên, M. L. Nielsen, H. Niederhausen, M. U. Nisa, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, M. Oehler, A. Olivas, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, P. Peiffer, C. Pérez de los Heros, S. Philippen, D. Pieloth, S. Pieper, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, P. B. Price, G. T. Przybylski, C. Raab, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, A. Rehman, R. Reimann, M. Renschler, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Scharf, M. Schaufel, H. Schieler, P. Schlunder, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, S. Sclafani, D. Seckel, S. Seunarine, S. Shefali, M. Silva, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, R. G. Stokstad, N. L. Strotjohann, T. Stuttard, G. W. Sullivan, I. Taboada, F. Tenholt, S. Ter-Antonyan, S. Tilav, F. Tischbein, K. Tollefson, L. Tomankova, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, C. F. Turley, J. P. Twagirayezu, B. Ty, E. Unger, M. A. Unland Elorrieta, J. Vandenbroucke, D. van Eijk, N. van Eijndhoven, D. Vannerom, J. van Santen, S. Verpoest, M. Vraeghe, C. Walck, A. Wallace, T. B. Watson, C. Weaver, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, B. J. Whelan, N. Whitehorn, K. Wiebe, C. H. Wiebusch, D. R. Williams, M. Wolf, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, Y. Xu, J. P. Yanez, S. Yoshida, T. Yuan, and Z. Zhang [hide authors].
Since the discovery of a flux of high-energy astrophysical neutrinos,
searches for their origins have focused primarily at TeV-PeV energies. Compared
to sub-TeV searches, high-energy searches benefit from an increase in the
neutrino cross section, improved angular resolution on the neutrino direction,
and a reduced background from atmospheric neutrinos and muons. However, the
focus on high energy does not preclude the existence of sub-TeV neutrino
emission where IceCube retains sensitivity. Here we present the first
all-flavor search from IceCube for transient emission of low-energy neutrinos,
focusing on the energy region of 5.6-100 GeV using three years of data obtained
with the IceCube-DeepCore detector. We find no evidence of transient neutrino
emission in the data, thus leading to a constraint on the volumetric rate of
astrophysical transient sources in the range of $\sim 705-2301\,
\text{Gpc}^{-3}\, \text{yr}^{-1}$ for sources following a subphotospheric
energy spectrum with a mean energy of 100 GeV and a bolometric energy of
$10^{52}$ erg.
Measurement of the high-energy all-flavor neutrino-nucleon cross section
with IceCube
2011.03560 [abs] [pdf]
[abstract]
by R. Abbasi, [and 364 more]M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, V. Basu, V. Baum, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Bourbeau, F. Bradascio, J. Braun, S. Bron, J. Brostean-Kaiser, A. Burgman, R. S. Busse, M. A. Campana, C. Chen, D. Chirkin, S. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, P. Dave, C. De Clercq, J. J. DeLaunay, H. Dembinski, K. Deoskar, S. De Ridder, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, S. Dharani, A. Diaz, J. C. Díaz-Vélez, H. Dujmovic, M. Dunkman, M. A. DuVernois, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, J. Evans, P. A. Evenson, S. Fahey, A. R. Fazely, S. Fiedlschuster, A. T. Fienberg, K. Filimonov, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, S. Garrappa, L. Gerhardt, A. Ghadimi, T. Glauch, T. Glüsenkamp, A. Goldschmidt, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, Z. Griffith, S. Griswold, M. Gündüz, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, M. Ha Minh, K. Hanson, J. Hardin, A. Haungs, S. Hauser, D. Hebecker, K. Helbing, F. Henningsen, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, T. Hoinka, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, B. J. P. Jones, R. Joppe, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, J. Kim, K. Kin, T. Kintscher, J. Kiryluk, S. R. Klein, R. Koirala, H. Kolanoski, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, K. Krings, G. Krückl, N. Kulacz, N. Kurahashi, A. Kyriacou, C. Lagunas Gualda, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, K. Leonard, A. Leszczyńska, Y. Li, Q. R. Liu, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, P. Mallik, S. Mancina, I. C. Mariş, R. Maruyama, K. Mase, F. McNally, K. Meagher, A. Medina, M. Meier, S. Meighen-Berger, J. Merz, J. Micallef, D. Mockler, G. Momenté, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, R. Naab, R. Nagai, U. Naumann, J. Necker, G. Neer, L. V. Nguyen, H. Niederhausen, M. U. Nisa, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, M. Oehler, A. Olivas, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, P. Peiffer, C. Pérez de los Heros, S. Philippen, D. Pieloth, S. Pieper, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, P. B. Price, G. T. Przybylski, C. Raab, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, A. Rehman, R. Reimann, M. Renschler, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Scharf, M. Schaufel, H. Schieler, P. Schlunder, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, S. Sclafani, D. Seckel, S. Seunarine, S. Shefali, M. Silva, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, R. G. Stokstad, N. L. Strotjohann, T. Stuttard, G. W. Sullivan, I. Taboada, F. Tenholt, S. Ter-Antonyan, S. Tilav, F. Tischbein, K. Tollefson, L. Tomankova, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, C. F. Turley, J. P. Twagirayezu, B. Ty, E. Unger, M. A. Unland Elorrieta, M. Usner, J. Vandenbroucke, D. van Eijk, N. van Eijndhoven, D. Vannerom, J. van Santen, S. Verpoest, M. Vraeghe, C. Walck, A. Wallace, N. Wandkowsky, T. B. Watson, C. Weaver, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, B. J. Whelan, N. Whitehorn, K. Wiebe, C. H. Wiebusch, D. R. Williams, M. Wolf, T. R. Wood, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, Y. Xu, J. P. Yanez, S. Yoshida, T. Yuan, and Z. Zhang [hide authors].
The flux of high-energy neutrinos passing through the Earth is attenuated due
to their interactions with matter. The interaction rate is modulated by the
neutrino interaction cross section and affects the flux arriving at the IceCube
Neutrino Observatory, a cubic-kilometer neutrino detector embedded in the
Antarctic ice sheet. We present a measurement of the neutrino cross section
between 60 TeV and 10 PeV using the high-energy starting events (HESE) sample
from IceCube with 7.5 years of data. The result is binned in neutrino energy
and obtained using both Bayesian and frequentist statistics. We find it
compatible with predictions from the Standard Model. Flavor information is
explicitly included through updated morphology classifiers, proxies for the the
three neutrino flavors. This is the first such measurement to use the three
morphologies as observables and the first to account for neutrinos from tau
decay.
The IceCube high-energy starting event sample: Description and flux
characterization with 7.5 years of data
2011.03545 [abs] [pdf]
[abstract]
by R. Abbasi, [and 365 more]M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, V. Basu, V. Baum, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Bourbeau, F. Bradascio, J. Braun, S. Bron, J. Brostean-Kaiser, A. Burgman, R. S. Busse, M. A. Campana, C. Chen, D. Chirkin, S. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, P. Dave, C. De Clercq, J. J. DeLaunay, H. Dembinski, K. Deoskar, S. De Ridder, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, S. Dharani, A. Diaz, J. C. Díaz-Vélez, H. Dujmovic, M. Dunkman, M. A. DuVernois, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, J. Evans, P. A. Evenson, S. Fahey, A. R. Fazely, S. Fiedlschuster, A. T. Fienberg, K. Filimonov, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, S. Garrappa, L. Gerhardt, A. Ghadimi, T. Glauch, T. Glüsenkamp, A. Goldschmidt, J. G. Gonzalez, S. Goswami, D. Grant, T. Grégoire, Z. Griffith, S. Griswold, M. Gündüz, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, M. Ha Minh, K. Hanson, J. Hardin, A. Haungs, S. Hauser, D. Hebecker, K. Helbing, F. Henningsen, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, T. Hoinka, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, B. J. P. Jones, R. Joppe, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, T. Karg, M. Karl, A. Karle, T. Katori, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, J. Kim, K. Kin, T. Kintscher, J. Kiryluk, S. R. Klein, R. Koirala, H. Kolanoski, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, K. Krings, G. Krückl, N. Kulacz, N. Kurahashi, A. Kyriacou, C. Lagunas Gualda, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, K. Leonard, A. Leszczyńska, Y. Li, Q. R. Liu, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, P. Mallik, S. Mancina, S. Mandalia, I. C. Mariş, R. Maruyama, K. Mase, F. McNally, K. Meagher, A. Medina, M. Meier, S. Meighen-Berger, J. Merz, J. Micallef, D. Mockler, G. Momenté, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, R. Naab, R. Nagai, U. Naumann, J. Necker, G. Neer, L. V. Nguyen, H. Niederhausen, M. U. Nisa, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, M. Oehler, A. Olivas, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, P. Peiffer, C. Pérez de los Heros, S. Philippen, D. Pieloth, S. Pieper, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, P. B. Price, G. T. Przybylski, C. Raab, A. Raissi, M. Rameez, K. Rawlins, I. C. Rea, A. Rehman, R. Reimann, M. Renschler, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Scharf, M. Schaufel, H. Schieler, P. Schlunder, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, S. Sclafani, D. Seckel, S. Seunarine, S. Shefali, M. Silva, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, R. G. Stokstad, N. L. Strotjohann, T. Stuttard, G. W. Sullivan, I. Taboada, F. Tenholt, S. Ter-Antonyan, S. Tilav, F. Tischbein, K. Tollefson, L. Tomankova, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, C. F. Turley, J. P. Twagirayezu, B. Ty, E. Unger, M. A. Unland Elorrieta, J. Vandenbroucke, D. van Eijk, N. van Eijndhoven, D. Vannerom, J. van Santen, S. Verpoest, M. Vraeghe, C. Walck, A. Wallace, N. Wandkowsky, T. B. Watson, C. Weaver, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, B. J. Whelan, N. Whitehorn, K. Wiebe, C. H. Wiebusch, D. R. Williams, M. Wolf, T. R. Wood, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, Y. Xu, J. P. Yanez, S. Yoshida, T. Yuan, and Z. Zhang [hide authors].
The IceCube Neutrino Observatory has established the existence of a
high-energy all-sky neutrino flux of astrophysical origin. This discovery was
made using events interacting within a fiducial region of the detector
surrounded by an active veto and with reconstructed energy above 60 TeV,
commonly known as the high-energy starting event sample, or HESE. We revisit
the analysis of the HESE sample with an additional 4.5 years of data, newer
glacial ice models, and improved systematics treatment. This paper describes
the sample in detail, reports on the latest astrophysical neutrino flux
measurements, and presents a source search for astrophysical neutrinos. We give
the compatibility of these observations with specific isotropic flux models
proposed in the literature as well as generic power-law-like scenarios.
Assuming $\nu_e:\nu_\mu:\nu_\tau=1:1:1$, and an equal flux of neutrinos and
antineutrinos, we find that the astrophysical neutrino spectrum is compatible
with an unbroken power law, with a preferred spectral index of
${2.87}^{+0.20}_{-0.19}$ for the $68.3\%$ confidence interval.
Intimate Relationship Between Sterile Neutrino Dark Matter and $Δ
N_{\rm eff}$
2011.02487 [abs] [pdf]
[abstract]
by Kevin J. Kelly, Manibrata Sen, and Yue Zhang.
The self-interacting neutrino hypothesis is well motivated for addressing the
tension between the origin of sterile neutrino dark matter and indirect
detection constraints. It can also result in a number of testable signals from
the laboratories to the cosmos. We explore a model of neutrino self-interaction
mediated by a Majoron-like scalar with sub-MeV mass, and show that explaining
the relic density of sterile neutrino dark matter implies a lower bound on the
amount of extra radiation in early universe, in particular $\Delta N_{\rm
eff}>0.12$ at the CMB epoch. This lower bound will be further strengthened with
an improved $X$-ray search at the Athena observatory. Such an intimate
relationship will be unambiguously tested by the upcoming CMB-S4 project.
Neutrino experiments probe hadrophilic light dark matter
2011.01939 [abs] [pdf]
[abstract]
by Yohei Ema, Filippo Sala, and Ryosuke Sato.
We use Super-K data to place new strong limits on interactions of sub-GeV
Dark Matter (DM) with nuclei, that rely on the DM flux inevitably induced by
cosmic-ray upscatterings. We derive analogous sensitivities at Hyper-K and DUNE
and compare them with others, e.g. at JUNO. Using simplified models, we find
that our proposal tests genuinely new parameter space, allowed both by
theoretical consistency and by other direct detection experiments, cosmology,
meson decays and our recast of monojet. Our results thus motivate and shape a
new physics case for any large volume detector sensitive to nuclear recoils.
Invisible neutrino decay in precision cosmology
2011.01502 [abs] [pdf]
[abstract]
by Gabriela Barenboim, [and 5 more]Joe Zhiyu Chen, Steen Hannestad, Isabel M. Oldengott, Thomas Tram, and Yvonne Y. Y. Wong [hide authors].
We revisit the topic of invisible neutrino decay in the precision
cosmological context, via a first-principles approach to understanding the
cosmic microwave background and large-scale structure phenomenology of such a
non-standard physics scenario. Assuming an effective Lagrangian in which a
heavier standard-model neutrino $\nu_H$ couples to a lighter one $\nu_l$ and a
massless scalar particle $\phi$ via a Yukawa interaction, we derive from first
principles the complete set of Boltzmann equations, at both the spatially
homogeneous and the first-order inhomogeneous levels, for the phase space
densities of $\nu_H$, $\nu_l$, and $\phi$ in the presence of the relevant decay
and inverse decay processes. With this set of equations in hand, we perform a
critical survey of recent works on cosmological invisible neutrino decay in
both limits of decay while $\nu_H$ is ultra-relativistic and non-relativistic.
Our two main findings are: (i) in the non-relativistic limit, the effective
equations of motion used to describe perturbations in the neutrino--scalar
system in the existing literature formally violate momentum conservation and
gauge invariance, and (ii) in the ultra-relativistic limit, exponential damping
of the anisotropic stress does not occur at the commonly-used rate $\Gamma_{\rm
T} =(1/\tau_0) (m_{\nu H}/E_{\nu H})^3$, but at a rate $\sim (1/\tau_0) (m_{\nu
H}/E_{\nu H})^5$. Both results are model-independent. The impact of the former
finding on the cosmology of invisible neutrino decay is likely small. The
latter, however, implies a significant revision of the cosmological limit on
the neutrino lifetime $\tau_0$ from $\tau_0^{\rm old} \gtrsim 1.2 \times 10^9\,
{\rm s}\, (m_{\nu H}/50\, {\rm meV})^3$ to $\tau_0 \gtrsim (4 \times 10^5 \to 4
\times 10^6)\, {\rm s}\, (m_{\nu H}/50 \, {\rm meV})^5$.
Neutrino 2020: Theory Outlook
2011.01264 [abs] [pdf]
[abstract]
by Goran Senjanovic.
I present a personal vision of what is essential in the field of neutrino
mass, both from the point of view of what has been achieved and what could lie
ahead. In the process, I offer a logical, theoretical and phenomenological
rationale behind my opinions. It is however neither a summary of what was
discussed in the conference nor a party-line viewpoint, rather an attempt to
dig through the enormous body of material in our field in order to uncover a
common unifying thread. The main focus is on the search for a predictive and
self-contained theory of the origin and nature of neutrino mass, with the
conclusion that the Left-Right Symmetric Model plays a special role in this
aspect.
Uncovering Majorana nature through a precision measurement of $CP$ phase
2011.01254 [abs] [pdf]
[abstract]
by J. C. Carrasco-Martínez, F. N. Díaz, and A. M. Gago.
We show the possibility to discover the neutrino nature by measuring the
Majorana CP phase at the DUNE experiment. This phase is turned on by a
decoherence environment, possibly originated by physics at the Planck scale. A
sizable distortion in the measurement of the Dirac CP violation phase
$\delta_{\mathrm{CP}}$ is observed at DUNE when compared with T2HK measurement
due to decoherence and non-null Majorana phase. Being that, when the
measurement of the Majorana phase is performed at DUNE, it reaches a precision
of 23 (21) $\%$ for a decoherence parameter $\Gamma=4.5(5.5)\times 10^{-24}
\mathrm{GeV}$ and a Majorana phase equal to $1.5 \pi$. The latter precision is
similar to the one obtained at the T2K experiment at its current Dirac CP
violation phase measurement.
A Non-Degenerate Neutrino Mass Signature in the Galaxy Bispectrum
2011.00899 [abs] [pdf]
[abstract]
by Farshad Kamalinejad and Zachary Slepian.
In the Standard Model, neutrinos are massless, yet oscillation experiments
show in fact they do have a small mass. Currently only the differences of the
masses' squares are known, and an upper bound on the sum. However, upcoming
surveys of the Universe's large-scale structure (LSS) can probe the neutrino
mass by exposing how neutrinos modulate galaxy clustering. But these
measurements are challenging: in looking at the clustering of galaxy pairs, the
effect of neutrinos is degenerate with galaxy formation, the details of which
are unknown. Marginalizing over them degrades the constraints. Here we show
that using correlations of galaxy triplets---the 3-Point Correlation Function
or its Fourier-space analog the bispectrum---can break the degeneracy between
galaxy formation physics (known as biasing) and the neutrino mass.
Specifically, we find a signature of neutrinos in the bispectrum's dipole
moment (with respect to triangle opening angle) that is roughly orthogonal to
the contribution of galaxy biases. This signature was missed in previous works
by failing to account for how neutrinos alter mode-coupling between
perturbations on different scales. Our proposed signature will contribute to
upcoming LSS surveys' such as DESI making a robust detection of the neutrino
mass. We estimate that it can offer several-$\sigma$ evidence for non-zero
$m_{\nu}$ with DESI from the bispectrum alone, and that this is independent
from information in the galaxy power spectrum.
October 2020
Constraints on elastic neutrino nucleus scattering in the fully coherent
regime from the CONUS experiment
2011.00210 [abs] [pdf]
[abstract]
by H. Bonet, [and 11 more]A. Bonhomme, C. Buck, K. Fülber, J. Hakenmüller, G. Heusser, T. Hugle, M. Lindner, W. Maneschg, T. Rink, H. Strecker, and R. Wink [hide authors].
We report the best limit on coherent elastic scattering of electron
antineutrinos emitted from a nuclear reactor off germanium nuclei. The
measurement was performed with the CONUS detectors positioned at 17.1m from the
3.9GWth reactor core of the nuclear power plant in Brokdorf, Germany. The
antineutrino energies of less than 10 MeV assure interactions in the fully
coherent regime. The analyzed dataset includes 248.7 kgd with the reactor
turned on and background data of 58.8 kgd with the reactor off. With a
quenching parameter of k = 0.18 for germanium, we determined an upper limit on
the number of neutrino events of 85 in the region of interest at 90% confidence
level. This new CONUS dataset disfavors quenching parameters above k = 0.27,
under the assumption of standard-model-like coherent scattering of the reactor
antineutrinos.
Tentative sensitivity of future $0νββ$-decay experiments to
neutrino masses and Majorana CP phases
2010.16281 [abs] [pdf]
[abstract]
by Guo-yuan Huang and Shun Zhou.
In the near future, the neutrinoless double-beta ($0\nu\beta\beta$) decay
experiments will hopefully reach the sensitivity of a few ${\rm meV}$ to the
effective neutrino mass $|m^{}_{\beta\beta}|$. In this paper, we tentatively
examine the sensitivity of future $0\nu\beta\beta$-decay experiments to
neutrino masses and Majorana CP phases by following the Bayesian statistical
approach. Provided experimental setups corresponding to the sensitivity of
$|m^{}_{\beta\beta}| \simeq 1~{\rm meV}$, the null observation of
$0\nu\beta\beta$ decays in the case of normal neutrino mass ordering leads to a
very competitive bound on the lightest neutrino mass $m^{}_1$. Namely, the
$95\%$ credible interval turns out to be $1.6~{\rm meV} \lesssim m^{}_1
\lesssim 7.3~{\rm meV}$ or $0.3~{\rm meV} \lesssim m^{}_1 \lesssim 5.6~{\rm
meV}$ when the uniform prior on $m^{}_1/{\rm eV}$ or on
$\log^{}_{10}(m^{}_1/{\rm eV})$ is adopted. Moreover, one of two Majorana CP
phases is strictly constrained, i.e., $140^\circ \lesssim \rho \lesssim
220^\circ$ for both priors of $m^{}_1$. In contrast, if a relatively worse
sensitivity of $|m^{}_{\beta\beta}| \simeq 10~{\rm meV}$ is assumed, the
constraint becomes accordingly $0.6~{\rm meV} \lesssim m^{}_1 \lesssim 26~{\rm
meV}$ or $0 \lesssim m^{}_1 \lesssim 6.1~{\rm meV}$, while two Majorana CP
phases will be essentially unconstrained. In the same statistical framework,
the prospects for the determination of neutrino mass ordering and the
discrimination between Majorana and Dirac nature of massive neutrinos in the
$0\nu\beta\beta$-decay experiments are also discussed. Given the experimental
sensitivity of $|m^{}_{\beta\beta}| \simeq 10~{\rm meV}$ (or $1~{\rm meV}$),
the strength of evidence to exclude the Majorana nature under the null
observation of $0\nu\beta\beta$ decays is found to be inconclusive (or strong),
no matter which of two priors on $m^{}_1$ is taken.
Constraining primordial black holes as dark matter at JUNO
2010.16053 [abs] [pdf]
[abstract]
by Sai Wang, [and 4 more]Dong-Mei Xia, Xukun Zhang, Shun Zhou, and Zhe Chang [hide authors].
As an attractive candidate for dark matter, the primordial black holes (PBHs)
in the mass range ($10^{15} \sim 10^{16}$)$\mathrm{g}$ could be detected via
their Hawking radiation, including neutrinos and antineutrinos of three
flavors. In this paper, we investigate the possibility to constrain the PBH as
dark matter by measuring (anti)neutrino signals at the large
liquid-scintillator detector of Jiangmen Underground Neutrino Observatory
(JUNO). Among six available detection channels, the inverse beta decay
$\overline{\nu}^{}_e + p \to e^+ + n$ is shown to be most sensitive to the
fraction $f^{}_{\rm PBH}$ of PBHs contributing to the dark matter abundance.
Given the PBH mass $M^{}_{\rm PBH} = 10^{15}~{\rm g}$, we find that JUNO will
be able to place an upper bound $f^{}_{\rm PBH} \lesssim 3\times 10^{-5}$,
which is 20 times better than the current best limit $f^{}_{\rm PBH} \lesssim
6\times 10^{-4}$ from Super-Kamiokande. For heavier PBHs with a lower Hawking
temperature, the (anti)neutrinos become less energetic, leading to a relatively
weaker bound.
No-go limitations on UV completions of the Neutrino Option
2010.15428 [abs] [pdf]
[abstract]
by Ilaria Brivio, Jim Talbert, and Michael Trott.
We discuss the possible origin of the Majorana mass scale(s) required for the
"Neutrino Option" where the electroweak scale is generated simultaneously with
light neutrino masses in a type-I seesaw model, by common dimension four
interactions. We establish no-go constraints on the perturbative generation of
the Majorana masses required due to global symmetries of the seesaw Lagrangian.
Astrophysical constraints on non-standard coherent neutrino-nucleus
scattering
2010.14545 [abs] [pdf]
[abstract]
by Anna M. Suliga and Irene Tamborra.
The exciting possibility of detecting supernova, solar, and atmospheric
neutrinos with coherent neutrino-nucleus scattering detectors is within reach,
opening up new avenues to probe New Physics. We explore the possibility of
constraining non-standard coherent neutrino-nucleus scattering through
astrophysical neutrinos. Sensitivity bounds on the mass and coupling of the new
mediator are obtained by inspecting the modifications induced by the new
interaction on the recoil rate observable in the upcoming RES-NOVA and DARWIN
facilities. Under the assumption of optimal background tagging, the detection
of neutrinos from a galactic supernova burst, or one-year exposure to solar and
atmospheric neutrinos, will place the most stringent bounds for mediator
couplings $g \gtrsim 10^{-5}$ and mediator masses between 1 and 100 MeV. A
similar, but slightly improved, potential to COHERENT will be provided for
larger mediator masses. In particular, RES-NOVA and DARWIN may potentially
provide one order of magnitude tighter constraints than XENON1T on the mediator
coupling. Non-standard coherent neutrino-nucleus scattering may also force
neutrinos to be trapped in the supernova core; this argument allows to probe
the region of the parameter space with $g \gtrsim 10^{-4}$, which is currently
excluded by other coherent neutrino-nucleus scattering facilities or other
astrophysical and terrestrial constraints.
Sensitivities of future reactor and long-baseline neutrino experiments
to NSI
2010.12849 [abs] [pdf]
[abstract]
by Pouya Bakhti and Meshkat Rajaee.
We investigate the potential of the next generation long-baseline neutrino
experiments DUNE and T2HK as well as the upcoming reactor experiment JUNO to
constrain Non-Standard Interaction (NSI) parameters. JUNO is going to provide
the most precise measurements of solar neutrino oscillation parameters as well
as determining the neutrino mass ordering. We study how the results of JUNO
combined with those of long-baseline neutrino experiments such as DUNE and T2HK
can help to determine oscillation parameters and to constrain NSI parameters.
We present excluded regions in NSI parameter space, $\epsilon_{\alpha \beta}$
assuming Standard Model (SM) as the null hypothesis. We further explore the
correlations between the NSI parameters and CP-violation phase.
New Solutions for Rotating Boson Stars
2010.09880 [abs] [pdf]
[abstract]
by Felix Kling, Arvind Rajaraman, and Freida Liz Rivera.
It has been shown that scalar fields can form gravitationally bound compact
objects called boson stars. In this study, we analyze boson star configurations
where the scalar fields contain a small amount of angular momentum and find two
new classes of solutions. In the first case all particles are in the same
slowly rotating state and in the second case the majority of particles are in
the non-rotating ground state and a small number of particles are in an excited
rotating state. In both cases, we solve the underlying Gross-Pitaevskii-Poisson
equations that describe the profile of these compact objects both numerically
as well as analytically through series expansions.
Rotations of the polarization of a gravitational wave propagating in
Universe
2010.09224 [abs] [pdf]
[abstract]
by Jia-Xi Feng, Fu-Wen Shu, and Anzhong Wang.
In this paper, we study the polarization of a gravitational wave (GW) emitted
by an astrophysical source at a cosmic distance propagating through the
Friedmann-Lema\^itre-Robertson-Walk universe. By considering the null geodesic
deviations, we first provide a definition of the polarization of the GW in
terms of the Weyl scalars with respect to a parallelly-transported frame along
the null geodesics, and then show explicitly that, due to different effects of
the expansion of the universe on the two polarization modes, the so-called "+"
and "$\times$" modes, the polarization angle of the GW changes generically,
when it is propagating through the curved background. By direct computations of
the polarization angle, we show that different epochs, radiation-, matter- and
$\Lambda$-dominated, have different effects on the polarization. In particular,
for a GW emitted by a binary system, we find explicitly the relation between
the change of the polarization angle $|\Delta \varphi|$ and the redshift $z_s$
of the source in different epochs. In the $\Lambda$CDM model, we find that the
order of $|\Delta \varphi|{\eta_0 F}$ is typically $O(10^{-3})$ to $O(10^3)$,
depending on the values of $z_s$, where $\eta_0$ is the (comoving) time of the
current universe, and
$F\equiv\Big(\frac{5}{256}\frac{1}{\tau_{obs}}\Big)^{3/8}\left(G_NM_c\right)^{-5/8}$
with $\tau_{obs}$ and $M_c$ being, respectively, the time to coalescence in the
observer's frame and the chirp mass of the binary system.
Neutrino oscillations in matter: from microscopic to macroscopic
description
2010.07847 [abs] [pdf]
[abstract]
by Evgeny Akhmedov.
Neutrino flavour transmutations in nonuniform matter are described by a
Schr\"{o}dinger-like evolution equation with coordinate-dependent potential. In
all the derivations of this equation it is assumed that the potential, which is
due to coherent forward scattering of neutrinos on matter constituents, is a
continuous function of coordinate that changes slowly over the distances of the
order of the neutrino de Broglie wavelength. This tacitly assumes that some
averaging of the microscopic potential (which takes into account the discrete
nature of the scatterers) has been performed.The averaging, however, must be
applied to the microscopic evolution equation as a whole and not just to the
potential. Such an averaging has never been explicitly carried out. We fill
this gap by considering the transition from the microscopic to macroscopic
neutrino evolution equation through a proper averaging procedure. We discuss
some subtleties related to this procedure and establish the applicability
domain of the standard macroscopic evolution equation. This, in particular,
allows us to answer the question of when neutrino propagation in rarefied media
(such as e.g.\ low-density gases or interstellar or intergalactic media) can be
considered within the standard theory of neutrino flavour evolution in matter.
Astronomy with energy dependent flavour ratios of extragalactic
neutrinos
2010.07336 [abs] [pdf]
[abstract]
by Siddhartha Karmakar, Sujata Pandey, and Subhendu Rakshit.
High energy astrophysical neutrinos interacting with ultralight dark matter
(DM) can undergo flavour oscillations that induce an energy dependence in the
flavour ratios. Such a dependence on the neutrino energy will reflect in the
track to shower ratio in neutrino telescopes like IceCube or KM3NeT. This opens
up a possibility to study DM density profiles of astrophysical objects like
AGN, GRB etc., which are the suspected sources of such neutrinos.
Charged Higgs effects in IceCube: PeV events and NSIs
2010.05797 [abs] [pdf]
[abstract]
by Ujjal Kumar Dey, Newton Nath, and Soumya Sadhukhan.
Extensions of the Standard Model with charged Higgs, having a non-negligible
coupling with neutrinos, can have interesting implications vis-\`{a}-vis
neutrino experiments. Such models can leave their footprints in the ultra-high
energy neutrino detectors like IceCube in the form of neutrino non-standard
interactions (NSIs) which can also be probed in lower energy neutrino
experiments. We consider a model based on the neutrinophilic two-Higgs doublets
and study its imprints in the recently reported excess neutrino events in the
PeV energy bins at the IceCube. An additional signature of the model is that it
also leads to sizeable NSIs. We perform a combined study of the latest IceCube
data along with various other constraints arising from neutrino experiments
e.g., Borexino, TEXONO, COHERENT, DUNE, and T2HK, together with the limits set
by the LEP experiment, and explore the parameter space which can lead to a
sizeable NSI.
Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background
2010.04728 [abs] [pdf]
[abstract]
by Daniel Kresse, Thomas Ertl, and Hans-Thomas Janka.
The diffuse cosmic supernova neutrino background (DSNB) is observational
target of the gadolinium-loaded Super-Kamiokande (SK) detector and the
forthcoming JUNO and Hyper-Kamiokande detectors. Current predictions are
hampered by our still incomplete understanding of the supernova (SN) explosion
mechanism and of the neutron star (NS) equation of state and maximum mass. In
our comprehensive study we revisit this problem on grounds of the landscapes of
successful and failed SN explosions obtained by Sukhbold et al. and Ertl et al.
with parametrized one-dimensional neutrino engines for large sets of
single-star and helium-star progenitors, with the latter serving as proxy of
binary evolution effects. Besides considering engines of different strengths,
leading to different fractions of failed SNe with black-hole (BH) formation, we
also vary the NS mass limit, the spectral shape of the neutrino emission, and
include contributions from poorly understood alternative NS-formation channels
such as accretion-induced or merger-induced collapse events. Since the neutrino
signals of our large model sets are approximate, we calibrate the associated
degrees of freedom by using state-of-the-art simulations of proto-neutron star
cooling. Our predictions are higher than other recent ones because of a large
fraction of failed SNe with long delay to BH formation. Our best-guess model
predicts a DSNB electron-antineutrino-flux of 28.8^{+24.6}_{-10.9}
cm^{-2}s^{-1} with 6.0^{+5.1}_{-2.1} cm^{-2}s^{-1} in the favorable measurement
interval of [10,30] MeV, and 1.3^{+1.1}_{-0.4} cm^{-2}s^{-1} with
electron-antineutrino energies > 17.3 MeV, which is roughly a factor of two
below the current SK limit. The uncertainty range is dominated by the still
insufficiently constrained cosmic rate of stellar core-collapse events.
Assessing the tension between a black hole dominated early universe and
leptogenesis
2010.03565 [abs] [pdf]
[abstract]
by Yuber F. Perez-Gonzalez and Jessica Turner.
We perform the first numerical calculation of the interplay between thermal
and black hole induced leptogenesis, demonstrating that the right-handed
neutrino surplus produced during the evaporation only partially mitigates the
entropy dilution suffered by the thermal component. As such, the
intermediate-mass regime of the right-handed neutrinos, $10^6{\rm~GeV} \lesssim
M_{N} \lesssim 10^{9}{\rm~GeV}$, could not explain the observed baryon
asymmetry even for fine-tuned scenarios if there existed a primordial black
hole dominated era, consistent with initial black hole masses of $M_i \gtrsim
\mathcal{O}\left(1\right)$ kg. Detection of the gravitational waves emitted
from the same primordial black holes would place intermediate-scale thermal
leptogenesis under tension.
September 2020
Exoplanets as Sub-GeV Dark Matter Detectors
2010.00015 [abs] [pdf]
[abstract]
by Rebecca K. Leane and Juri Smirnov.
We present exoplanets as new targets to discover Dark Matter (DM). Throughout
the Milky Way, DM can scatter, become captured, deposit annihilation energy,
and increase the heat flow within exoplanets. We estimate upcoming infrared
telescope sensitivity to this scenario, finding actionable discovery or
exclusion searches. We find that DM with masses above about an MeV can be
probed with exoplanets at DM-proton and DM-electron scattering cross sections
down to about $10^{-37}$cm$^2$, stronger than existing limits by up to six
orders of magnitude. Supporting evidence of a DM origin can be identified
through DM-induced exoplanet heating correlated with Galactic position, and
hence DM density. This provides new motivation to measure the temperature of
the billions of brown dwarfs, rogue planets, and gas giants peppered throughout
our Galaxy.
Neutrino oscillation in dark matter with $L_μ-L_τ$
2009.14703 [abs] [pdf]
[abstract]
by Wei Chao, [and 3 more]Yanyan Hu, Siyu Jiang, and Mingjie Jin [hide authors].
In this paper, we study the phenomenology of a Dirac dark matter in the
$L_\mu-L_\tau$ model and investigate the neutrino oscillation in the dark halo.
Since dark matter couples to the muon neutrino and the tau neutrino with
opposite sign couplings, it contributes effective potentials, $\pm A_\chi$, to
the evolution equation of the neutrino flavor transition amplitude, which can
be significant for high energy neutrino oscillations in a dense dark matter
environment. We discuss neutrino masses, lepton mixing angles, Dirac CP phase,
and neutrino oscillation probabilities in the dark halo using full numerical
calculations. Results show that neutrinos can endure very different matter
effects. When the potential $A_\chi$ becomes ultra-large, three neutrino
flavors decouple from each other.
Neutrino Oscillation Constraints on U(1)' Models: from Non-Standard
Interactions to Long-Range Forces
2009.14220 [abs] [pdf]
[abstract]
by Pilar Coloma, M. C. Gonzalez-Garcia, and Michele Maltoni.
We quantify the effect of gauge bosons from a weakly coupled lepton flavor
dependent $U(1)'$ interaction on the matter background in the evolution of
solar, atmospheric, reactor and long-baseline accelerator neutrinos in the
global analysis of oscillation data. The analysis is performed for interaction
lengths ranging from the Sun-Earth distance to effective contact neutrino
interactions. We survey $\sim 10000$ set of models characterized by the six
relevant fermion $U(1)'$ charges and find that in all cases, constraints on the
coupling and mass of the $Z'$ can be derived. We also find that about 5% of the
$U(1)'$ model charges lead to a viable LMA-D solution but this is only possible
in the contact interaction limit. We explicitly quantify the constraints for a
variety of models including $U(1)_{B-3L_e}$, $U(1)_{B-3L_\mu}$,
$U(1)_{B-3L_\tau}$, $U(1)_{B-\frac{3}{2}(L_\mu+L_\tau)}$, $U(1)_{L_e-L_\mu}$,
$U(1)_{L_e-L_\tau}$, $U(1)_{L_e-\frac{1}{2}(L_\mu+L_\tau)}$. We compare the
constraints imposed by our oscillation analysis with the strongest bounds from
fifth force searches, violation of equivalence principle as well as bounds from
scattering experiments and white dwarf cooling. Our results show that
generically, the oscillation analysis improves over the existing bounds from
gravity tests for $Z'$ lighter than $\sim 10^{-8} \to 10^{-11}$ eV depending on
the specific couplings. In the contact interaction limit, we find that for most
models listed above there are values of $g'$ and $M_{Z'}$ for which the
oscillation analysis provides constraints beyond those imposed by laboratory
experiments. Finally we illustrate the range of $Z'$ and couplings leading to a
viable LMA-D solution for two sets of models.
Experimental tests of sub-surface reflectors as an explanation for the
ANITA anomalous events
2009.13010 [abs] [pdf]
[abstract]
by D. Smith, [and 33 more]D. Z. Besson, C. Deaconu, S. Prohira, P. Allison, L. Batten, J. J. Beatty, W. R. Binns, V. Bugaev, P. Cao, C. Chen, P. Chen, J. M. Clem, A. Connolly, L. Cremonesi, P. Dasgupta, P. W. Gorham, M. H. Israel, T. C. Liu, A. Ludwig, S. Matsuno, C. Miki, J. Nam, A. Novikov, R. J. Nichol, E. Oberla, R. Prechelt, B. F. Rauch, J. Russell, D. Saltzberg, D. Seckel, G. S. Varner, A. G. Vieregg, and S. A. Wissel [hide authors].
The balloon-borne ANITA experiment is designed to detect ultra-high energy
neutrinos via radio emissions produced by an in-ice shower. Although initially
purposed for interactions within the Antarctic ice sheet, ANITA also
demonstrated the ability to self-trigger on radio emissions from ultra-high
energy charged cosmic rays interacting in the Earth's atmosphere. For showers
produced above the Antarctic ice sheet, reflection of the down-coming radio
signals at the Antarctic surface should result in a polarity inversion prior to
subsequent observation at the $\sim$35-40 km altitude ANITA gondola. ANITA has
published two anomalous instances of upcoming cosmic-rays with measured
polarity opposite the remaining sample of $\sim$50 UHECR signals. The steep
observed upwards incidence angles (25--30 degrees relative to the horizontal)
require non-Standard Model physics if these events are due to in-ice neutrino
interactions, as the Standard Model cross-section would otherwise prohibit
neutrinos from penetrating the long required chord of Earth. Shoemaker et al.
posit that glaciological effects may explain the steep observed anomalous
events. We herein consider the scenarios offered by Shoemaker et al. and find
them to be disfavored by extant ANITA and HiCal experimental data. We note that
the recent report of four additional near-horizon anomalous ANITA-4 events, at
$>3\sigma$ significance, are incompatible with their model, which requires
significant signal transmission into the ice.
Squeezing the Parameter Space for Lorentz Violation in the Neutrino
Sector by Additional Decay Channels
2009.11947 [abs] [pdf]
[abstract]
by Ulrich D. Jentschura.
The hypothesis of Lorentz violation in the neutrino sector has intrigued
scientists for the last two to three decades. A number of theoretical arguments
support the emergence of such violations first and foremost for neutrinos,
which constitute the "most elusive" and "least interacting" particles known to
mankind. It is of obvious interest to place stringent bounds on the
Lorentz-violating parameters in the neutrino sector. In the past, the most
stringent bounds have been placed by calculating the probability of neutrino
decay into a lepton pair, a process made kinematically feasible by Lorentz
violation in the neutrino sector, above a certain threshold. However, even more
stringent bounds can be placed on the Lorentz-violating parameters if one takes
into account, additionally, the possibility of neutrino splitting, i.e., of
neutrino decay into a neutrino of lower energy, accompanied by "neutrino-pair
Cerenkov radiation". This process has negligible threshold and can be used to
improve the bounds on Lorentz-violating parameters in the neutrino sector.
Finally, we take the opportunity to discuss the relation of Lorentz and gauge
symmetry breaking, with a special emphasis on the theoretical models employed
in our calculations.
Ejection of supermassive black holes and implications for merger rates
in fuzzy dark matter haloes
2009.10167 [abs] [pdf]
[abstract]
by Amr El-Zant, Zacharias Roupas, and Joseph Silk.
Fuzzy dark matter (FDM) consisting of ultra-light axions has been invoked to
alleviate galactic-scale problems in the cold dark matter scenario. FDM
fluctuations, created via the superposition of waves, can impact the motion of
a central supermassive black hole (SMBH) immersed in an FDM halo. The SMBH will
undergo a random walk, induced by FDM fluctuations, that can result in its
ejection from the central region. This effect is strongest in dwarf galaxies,
accounting for wandering SMBHs and the low detection rate of AGN in dwarf
spheroidal galaxies. In addition, a lower bound on the allowed axion masses is
inferred both for Sagittarius $A^*$ and heavier SMBH; to avoid ejection from
the galactic centres, axion masses of the order of $10^{-22}{\rm eV}$ or
lighter are excluded. Stronger limits are inferred for merging galaxies. We
find that the event rate of SMBH mergers in FDM haloes and the associated SMBH
growth rates can be reduced by at least an order of magnitude.
Imprints of Axion Superradiance in the CMB
2009.10074 [abs] [pdf]
[abstract]
by Diego Blas and Samuel J. Witte.
Light axions ($m_a \lesssim 10^{-10}$ eV) can form dense clouds around
rapidly rotating astrophysical black holes via a mechanism known as rotational
superradiance. The coupling between axions and photons induces a parametric
resonance, arising from the stimulated decay of the axion cloud, which can
rapidly convert regions of large axion number densities into an enormous flux
of low-energy photons. In this work we consider the phenomenological
implications of a superradiant axion cloud undergoing resonant decay. We show
that the low energy photons produced from such events will be absorbed over
cosmologically short distances, potentially inducing massive shockwaves that
heat and ionize the IGM over Mpc scales. These shockwaves may leave observable
imprints in the form of anisotropic spectral distortions or inhomogeneous
features in the optical depth.
Ultralight Bosonic Field Mass Bounds from Astrophysical Black Hole Spin
2009.07206 [abs] [pdf]
[abstract]
by Matthew J. Stott.
Black Hole measurements have grown significantly in the new age of
gravitation wave astronomy from LIGO observations of binary black hole mergers.
As yet unobserved massive ultralight bosonic fields represent one of the most
exciting features of Standard Model extensions, capable of providing solutions
to numerous paradigmatic issues in particle physics and cosmology. In this work
we explore bounds from spinning astrophysical black holes and their angular
momentum energy transfer to bosonic condensates which can form surrounding the
black hole via superradiant instabilities. Using recent analytical results we
perform a simplified analysis with a generous ensemble of black hole parameter
measurements where we find superradiance very generally excludes bosonic fields
in the mass ranges; spin-0: ${\scriptsize \{ 3.8\times10^{-14}\ {\rm eV} \leq
\mu_0 \leq 3.4\times10^{-11}\ {\rm eV}, 5.5\times10^{-20}\ {\rm eV} \leq \mu_0
\leq 1.3\times10^{-16}\ {\rm eV}, 2.5\times10^{-21}\ {\rm eV} \leq \mu_0 \leq
1.2\times10^{-20}\ {\rm eV}\}}$, spin-1: ${\scriptsize \{ 6.2\times10^{-15}\
{\rm eV} \leq \mu_1 \leq 3.9\times10^{-11}\ {\rm eV}, 2.8\times10^{-22}\ {\rm
eV} \leq \mu_1 \leq 1.9\times10^{-16}\ {\rm eV} \}}$ and spin-2: ${\scriptsize
\{ 2.2\times10^{-14}\ {\rm eV} \leq \mu_2 \leq 2.8\times10^{-11}\ {\rm eV},
1.8\times10^{-20}\ {\rm eV} \leq \mu_2 \leq 1.8\times10^{-16}\ {\rm eV},
6.4\times10^{-22}\ {\rm eV} \leq \mu_2 \leq 7.7\times10^{-21}\ {\rm eV} \}}$
respectively. We also explore these bounds in the context of specific
phenomenological models, specifically the QCD axion, M-theory models and fuzzy
dark matter sitting at the edges of current limits. In particular we include
recent measurements of event GW190521 and M87* used to constrain both the
masses and decay constants of axion like fields. Finally we comment a simple
example of a spectrum of fields for the spin-0 and spin-1 cases.
Constraints on neutrino non-standard interactions from LHC data with
large missing transverse momentum
2009.06668 [abs] [pdf]
[abstract]
by DianYu Liu, ChuanLe Sun, and Jun Gao.
The possible non-standard interactions (NSIs) of neutrinos with matter plays
important role in the global determination of neutrino properties. In our study
we select various data sets from LHC measurements at 13 TeV with integrated
luminosities of $35 \sim 139$ fb$^{-1}$, including production of a single jet,
photon, $W/Z$ boson, or charged lepton accompanied with large missing
transverse momentum. We derive constraints on neutral-current NSIs with quarks
imposed by different data sets in a framework of either effective operators or
simplified $Z'$ models. We use theoretical predictions of productions induced
by NSIs at next-to-leading order in QCD matched with parton showering which
stabilize the theory predictions and result in more robust constraints. In a
simplified $Z'$ model we obtain a 95% CLs upper limit on the conventional NSI
strength $\epsilon$ of 0.042 and 0.0028 for a $Z'$ mass of 0.2 and 2 TeV
respectively. We also discuss possible improvements from future runs of LHC
with higher luminosities.
Cosmic String Interpretation of NANOGrav Pulsar Timing Data
2009.06555 [abs] [pdf]
[abstract]
by John Ellis and Marek Lewicki.
Pulsar timing data used to provide upper limits on a possible stochastic
gravitational wave background (SGWB). However, the NANOGrav Collaboration has
recently reported strong evidence for a stochastic common-spectrum process,
which we interpret as a SGWB in the framework of cosmic strings. The possible
NANOGrav signal would correspond to a string tension $G\mu \in (4 \times
10^{-11}, 10^{-10}) $ at the 68% confidence level, with a different frequency
dependence from supermassive black hole mergers. The SGWB produced by cosmic
strings with such values of $G\mu$ would be beyond the reach of LIGO, but could
be measured by other planned and proposed detectors such as SKA, LISA, TianQin,
AION-1km, AEDGE, Einstein Telescope and Cosmic Explorer.
GW190521 as a merger of Proca stars: a potential new vector boson of
$8.7 \times 10^{-13}$ eV
2009.05376 [abs] [pdf]
[abstract]
by Juan Calderón Bustillo, [and 8 more]Nicolas Sanchis-Gual, Alejandro Torres-Forné, José A. Font, Avi Vajpeyi, Rory Smith, Carlos Herdeiro, Eugen Radu, and Samson H. W. Leong [hide authors].
Advanced LIGO-Virgo reported a short gravitational-wave signal (GW190521)
interpreted as a quasi-circular merger of black holes, one populating the
pair-instability supernova gap, forming a remnant black hole of $M_f\sim 142
M_\odot$ at a luminosity distance of $d_L \sim 5.3$ Gpc. With barely visible
pre-merger emission, however, GW190521 merits further investigation of the
pre-merger dynamics and even of the very nature of the colliding objects. We
show that GW190521 is consistent with numerically simulated signals from
head-on collisions of two (equal mass and spin) horizonless vector boson stars
(aka Proca stars), forming a final black hole with $M_f =
231^{+13}_{-17}\,M_\odot$, located at a distance of $d_L = 571^{+348}_{-181}$
Mpc. The favoured mass for the ultra-light vector boson constituent of the
Proca stars is $\mu_{\rm V}= 8.72^{+0.73}_{-0.82}\times10^{-13}$ eV. This
provides the first demonstration of close degeneracy between these two
theoretical models, for a real gravitational-wave event. Confirmation of the
Proca star interpretation, which we find statistically slightly preferred,
would provide the first evidence for a long sought dark matter particle.
Impact of high energy beam tunes on the sensitivities to the standard
unknowns at DUNE
2009.05061 [abs] [pdf]
[abstract]
by Jogesh Rout, [and 4 more]Samiran Roy, Mehedi Masud, Mary Bishai, and Poonam Mehta [hide authors].
Even though neutrino oscillations have been conclusively established, there
are a few unanswered questions pertaining to leptonic Charge Parity violation
(CPV), mass hierarchy (MH) and $\theta_{23}$ octant degeneracy. Addressing
these questions is of paramount importance at the current and future neutrino
experiments including the Deep Underground Neutrino Experiment (DUNE) which has
a baseline of 1300 km. In the standard mode, DUNE is expected to run with a
{\textit{low energy}} (LE) tuned beam which peaks around the first oscillation
maximum ($2-3$ GeV) (and then sharply falls off as we go to higher energies).
However, the wide band nature of the beam available at long baseline neutrino
facility (LBNF) allows for the flexibility in utilizing beam tunes that are
well-suited at higher energies as well. In this work, we utilize a beam that
provides high statistics at higher energies which is referred to as the
{\textit{medium energy}} (ME) beam. This opens up the possibility of exploring
not only the usual oscillation channels but also the $\nu_{\mu} \to \nu_{\tau}$
oscillation channel which was otherwise not accessible. Our goal is to find an
optimal combination of beam tune and runtime (with the total runtime held
fixed) distributed in neutrino and antineutrino mode that leads to an
improvement in the sensitivities of these parameters at DUNE. In our analysis,
we incorporate all the three channels ($\nu_{\mu} \to \nu_{e}, \nu_{\mu} \to
\nu_{\mu}, \nu_{\mu} \to \nu_{\tau}$) and develop an understanding of their
relative contributions in sensitivities at the level of $\Delta \chi^2$.
Finally, we obtain the preferred combination of runtime using both the beam
tunes as well as neutrino and antineutrino mode that lead to enhanced
sensitivity to the current unknowns in neutrino oscillation physics i.e., CPV,
MH and $\theta_{23}$ octant.
On the rate of core collapse supernovae in the Milky Way
2009.03438 [abs] [pdf]
[abstract]
by Karolina Rozwadowska, Francesco Vissani, and Enrico Cappellaro.
Several large neutrino telescopes, operating at various sites around the
world, have as their main objective the first detection of neutrinos emitted by
a gravitational collapse in the Milky Way. The success of these observation
programs depends on the rate of supernova core collapse in the Milky Way, $R$.
In this work, standard statistical techniques are used to combine several
independent results. Their consistency is discussed and the most critical input
data are identified. The inference on $R$ is further tested and refined by
including direct information on the occurrence rate of gravitational collapse
events in the Milky Way and in the Local Group, obtained from neutrino
telescopes and electromagnetic surveys. A conservative treatment of the errors
yields a combined rate $R=1.63 \pm 0.46$ (100 yr)$^{-1}$; the corresponding
time between core collapse supernova events turns out to be
$T=61_{-14}^{+24}$~yr. The importance to update the analysis of the stellar
birthrate method is emphasized.
Astrophysical hints for magnetic black holes
2009.03363 [abs] [pdf]
[abstract]
by Diptimoy Ghosh, Arun Thalapillil, and Farman Ullah.
We discuss a cornucopia of potential astrophysical signatures and constraints
on magnetically charged black holes of various masses. As recently highlighted,
being potentially viable astrophysical candidates with immense electromagnetic
fields, they may be ideal windows to fundamental physics, electroweak symmetry
restoration and non-perturbative quantum field theoretic phenomena. We
investigate various potential astrophysical pointers and bounds -- including
limits on charges, location of stable orbits and horizons in asymptotically
flat and asymptotically de Sitter backgrounds, bounds from galactic magnetic
fields and dark matter measurements, characteristic electromagnetic fluxes and
tell-tale gravitational wave emissions during binary inspirals. Stable orbits
around these objects hold an imprint of their nature and in the asymptotically
de Sitter case, there is also a qualitatively new feature with the emergence of
a stable outer orbit. We consider binary inspirals of both magnetic and
neutral, and magnetic and magnetic, black hole pairs. The electromagnetic
emissions and the gravitational waveform evolution, along with inter-black hole
separation, display distinct features. Many of the astrophysical signatures may
be observationally glaring -- for instance, even in regions of parameter space
where no electroweak corona forms, owing to magnetic fields that are still many
orders of magnitude larger than even Magnetars, their consequent
electromagnetic emissions will be spectacular during binary inspirals. While
adding new results, our discussions also complement works in similar contexts,
that have appeared recently in the literature.
Strengthening the bound on the mass of the lightest neutrino with
terrestrial and cosmological experiments
2009.03287 [abs] [pdf]
[abstract]
by The GAMBIT Cosmology Workgroup, [and 14 more]:, Patrick Stöcker, Csaba Balázs, Sanjay Bloor, Torsten Bringmann, Tomás E. Gonzalo, Will Handley, Selim Hotinli, Cullan Howlett, Felix Kahlhoefer, Janina J. Renk, Pat Scott, Aaron C. Vincent, and Martin White [hide authors].
We determine the upper limit on the mass of the lightest neutrino from the
most robust recent cosmological and terrestrial data. Marginalizing over
possible effective relativistic degrees of freedom at early times
($N_\mathrm{eff}$) and assuming normal mass ordering, the mass of the lightest
neutrino is less than 0.037 eV at 95% confidence; with inverted ordering, the
bound is 0.042 eV. These results improve upon the strength and robustness of
other recent limits and constrain the mass of the lightest neutrino to be
barely larger than the largest mass splitting. We show the impacts of realistic
mass models, and different sources of $N_\mathrm{eff}$.
Neutrino telescopes and high-energy cosmic neutrinos
2009.01919 [abs] [pdf]
[abstract]
by Andrea Palladino, Maurizio Spurio, and Francesco Vissani.
In this review paper, we present the main aspects of high-energy cosmic
neutrino astrophysics. We begin by describing the generic expectations for
cosmic neutrinos, including the effects of propagation from their sources to
the detectors. Then we introduce the operating principles of current neutrino
telescopes, and examine the main features (topologies) of the observable
events. After a discussion of the main background processes, due to the
concomitant presence of secondary particles produced in the terrestrial
atmosphere by cosmic rays, we summarize the current status of the observations
with astrophysical relevance that have been greatly contributed by IceCube
detector. Then, we examine various interpretations of these findings, trying to
assess the best candidate sources of cosmic neutrinos. We conclude with a brief
perspective on how the field could evolve within a few years.
August 2020
Search for sterile neutrino with light gauge interactions: recasting
collider, beam-dump, and neutrino telescope searches
2008.12598 [abs] [pdf]
[abstract]
by Yongsoo Jho, [and 3 more]Jongkuk Kim, Pyungwon Ko, and Seong Chan Park [hide authors].
We investigate features of the sterile neutrinos in the presence of a light
gauge boson $X^\mu$ that couples to the neutrino sector. The novel bounds on
the active-sterile neutrino mixings $| U_{\ell 4} |^2$, especially for tau
flavor ($l = \tau$), from various collider and fixed target experiments are
explored. Also, taking into account the additional decay channel of the sterile
neutrino into a light gauge boson ($\nu_4 \to \nu_\ell e^+ e^-$), we explore
and constrain a parameter space for low energy excess in neutrino oscillation
experiments.
Constraints on Decaying Sterile Neutrinos from Solar Antineutrinos
2008.11851 [abs] [pdf]
[abstract]
by Matheus Hostert and Maxim Pospelov.
Solar neutrino experiments are highly sensitive to sources of
$\nu\to\overline{\nu}$ conversions in the $^8$B neutrino flux. In this work we
adapt these searches to non-minimal sterile neutrino models recently proposed
to explain the LSND, MiniBooNE, and reactor anomalies. The production of such
sterile neutrinos in the Sun, followed the decay chain $\nu_4 \to \nu \phi \to
\nu \nu \overline{\nu}$ with a new scalar $\phi$ results in upper limits for
the neutrino mixing $|U_{e4}|^2$ at the per mille level. We conclude that a
simultaneous explanations of all anomalies is in tension with KamLAND,
Super-Kamiokande, and Borexino constraints on the flux of solar antineutrinos.
We then present other minimal models that violate parity or lepton number, and
discuss the applicability of our constraints in each case. Future improvements
can be expected from existing Borexino data as well as from future searches at
Super-Kamiokande with added Gd.
Synergies and Prospects for Early Resolution of the Neutrino Mass
Ordering
2008.11280 [abs] [pdf]
[abstract]
by Anatael Cabrera, [and 25 more]Yang Han, Michel Obolensky, Fabien Cavalier, João Coelho, Diana Navas Nicolás, Hiroshi Nunokawa, Laurent Simard, Jianming Bian, Nitish Nayak, Juan Pedro Ochoa-Ricoux, Bedřich Roskovec, Pietro Chimenti, Stefano Dusini, Mathieu Bongrand, Rebin Karaparambil, Victor Lebrin, Benoit Viaud, Frederic Yermia, Lily Asquith, Thiago J. C. Bezerra, Jeff Hartnell, Pierre Lasorak, Jiajie Ling, Jiajun Liao, and Hongzhao Yu [hide authors].
The measurement of neutrino Mass Ordering (MO) is a fundamental element for
the understanding of leptonic flavour sector of the Standard Model of Particle
Physics. Its determination relies on the precise measurement of $\Delta
m^2_{31}$ and $\Delta m^2_{32}$ using either neutrino vacuum oscillations, such
as the ones studied by medium baseline reactor experiments, or matter effect
modified oscillations such as those manifesting in long-baseline neutrino beams
(LB$\nu$B) or atmospheric neutrino experiments. Despite existing MO indication
today, a fully resolved MO measurement ($\geq$5$\sigma$) is most likely to
await for the next generation of neutrino experiments: JUNO, whose stand-alone
sensitivity is $\sim$3$\sigma$, or LB$\nu$B experiments (DUNE and
Hyper-Kamiokande). Upcoming atmospheric neutrino experiments are also expected
to provide precious information. In this work, we study the possible context
for the earliest full MO resolution. A firm resolution is possible even before
2028, exploiting mainly vacuum oscillation, upon the combination of JUNO and
the current generation of LB$\nu$B experiments (NOvA and T2K). This opportunity
is possible thanks to a powerful synergy boosting the overall sensitivity where
the sub-percent precision of $\Delta m^2_{32}$ by LB$\nu$B experiments is found
to be the leading order term for the MO earliest discovery. We also found that
the comparison between matter and vacuum driven oscillation results enables
unique discovery potential for physics beyond the Standard Model.
Multimessenger Gamma-Ray and Neutrino Coincidence Alerts using HAWC and
IceCube sub-threshold Data
2008.10616 [abs] [pdf]
[abstract]
by H. A. Ayala Solares, [and 449 more]S. Coutu, J. J. DeLaunay, D. B. Fox, T. Grégoire, A. Keivani, F. Krauß, M. Mostafá, K. Murase, C. F. Turley, A. Albert, R. Alfaro, C. Alvarez, J. R. Angeles Camacho, J. C. Arteaga-Velázquez, K. P. Arunbabu, D. Avila Rojas, E. Belmont-Moreno, C. Brisbois, K. S. Caballero-Mora, A. Carramiñana, S. Casanova, U. Cotti, E. De la Fuente, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, C. Espinoza, K. L. Fan, H. Fleischhack, N. Fraija, A. Galván-Gámez, D. Garcia, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, B. Hona, D. Huang, F. Hueyotl-Zahuantitla, P. Huntemeyer, A. Iriarte, A. Jardin-Blicq, V. Joshi, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, O. Martinez, I. Martinez-Castellanos, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, E. Moreno, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, A. Peisker, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, F. Salesa Greus, A. Sandoval, A. J. Smith, R. W. Springer, K. Tollefson, I. Torres, R. Torres-Escobedo, F. Ureña-Mena, L. Villaseñor, T. Weisgarber, E. Willox, A. Zepeda, H. Zhou, C. de León, M. G. Aartsen, R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, J. Auffenberg, S. Axani, H. Bagherpour, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, V. Basu, V. Baum, S. Baur, R. Bay, J. J. Beatty, K. -H. Becker, J. Becker Tjus, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, C. Bohm, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Bourbeau, F. Bradascio, J. Braun, S. Bron, J. Brostean-Kaiser, A. Burgman, J. Buscher, R. S. Busse, T. Carver, C. Chen, E. Cheung, D. Chirkin, S. Choi, B. A. Clark, K. Clark, L. Classen, A. Coleman, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, P. Dave, C. De Clercq, H. Dembinski, K. Deoskar, S. De Ridder, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, S. Dharani, A. Diaz, H. Dujmovic, M. Dunkman, E. Dvorak, T. Ehrhardt, P. Eller, R. Engel, P. A. Evenson, S. Fahey, A. R. Fazely, J. Felde, A. Fienberg, K. Filimonov, C. Finley, A. Franckowiak, E. Friedman, A. Fritz, T. K. Gaisser, J. Gallagher, E. Ganster, S. Garrappa, L. Gerhardt, T. Glauch, T. Glüsenkamp, A. Goldschmidt, J. G. Gonzalez, D. Grant, Z. Griffith, S. Griswold, M. Günder, M. Gündüz, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, K. Hanson, J. Hardin, A. Haungs, S. Hauser, D. Hebecker, D. Heereman, P. Heix, K. Helbing, R. Hellauer, F. Henningsen, S. Hickford, J. Hignight, C. Hill, G. C. Hill, K. D. Hoffman, R. Hoffmann, T. Hoinka, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, B. J. P. Jones, F. Jonske, R. Joppe, D. Kang, W. Kang, A. Kappes, D. Kappesser, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, M. Kellermann, J. L. Kelley, A. Kheirandish, J. Kim, K. Kin, T. Kintscher, J. Kiryluk, T. Kittler, S. R. Klein, R. Koirala, H. Kolanoski, L. Köpke, C. Kopper, S. Kopper, D. J. Koskinen, P. Koundal, M. Kowalski, K. Krings, G. Krückl, N. Kulacz, N. Kurahashi, A. Kyriacou, J. L. Lanfranchi, M. J. Larson, F. Lauber, J. P. Lazar, K. Leonard, A. Leszczyńska, Y. Li, Q. R. Liu, E. Lohfink, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, J. Lünemann, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, G. Maggi, K. B. M. Mahn, Y. Makino, P. Mallik, S. Mancina, I. C. Mariş, R. Maruyama, K. Mase, R. Maunu, F. McNally, K. Meagher, M. Medici, A. Medina, M. Meier, S. Meighen-Berger, J. Merz, T. Meures, J. Micallef, D. Mockler, G. Momenté, T. Montaruli, R. W. Moore, R. Morse, M. Moulai, P. Muth, R. Nagai, U. Naumann, G. Neer, L. V. Nguyen, H. Niederhausen, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, M. Oehler, A. Olivas, A. O'Murchadha, E. O'Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, P. Peiffer, C. Pérez de los Heros, S. Philippen, D. Pieloth, S. Pieper, E. Pinat, A. Pizzuto, M. Plum, Y. Popovych, A. Porcelli, M. Prado Rodriguez, P. B. Price, G. T. Przybylski, C. Raab, A. Raissi, M. Rameez, L. Rauch, K. Rawlins, I. C. Rea, A. Rehman, R. Reimann, B. Relethford, M. Renschler, G. Renzi, E. Resconi, W. Rhode, M. Richman, B. Riedel, S. Robertson, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, S. Sarkar, K. Satalecka, M. Scharf, M. Schaufel, H. Schieler, P. Schlunder, T. Schmidt, A. Schneider, J. Schneider, F. G. Schröder, L. Schumacher, S. Sclafani, D. Seckel, S. Seunarine, S. Shefali, M. Silva, B. Smithers, R. Snihur, J. Soedingrekso, D. Soldin, M. Song, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, R. G. Stokstad, N. L. Strotjohann, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, F. Tenholt, S. Ter-Antonyan, A. Terliuk, S. Tilav, L. Tomankova, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, M. Tselengidou, C. F. Tung, A. Turcati, R. Turcotte, B. Ty, E. Unger, M. A. Unland Elorrieta, M. Usner, J. Vandenbroucke, W. Van Driessche, D. van Eijk, N. van Eijndhoven, D. Vannerom, J. van Santen, S. Verpoest, M. Vraeghe, C. Walck, A. Wallace, M. Wallraff, T. B. Watson, C. Weaver, A. Weindl, M. J. Weiss, J. Weldert, C. Wendt, J. Werthebach, B. J. Whelan, N. Whitehorn, K. Wiebe, C. H. Wiebusch, D. R. Williams, L. Wills, M. Wolf, T. R. Wood, K. Woschnagg, G. Wrede, J. Wulff, X. W. Xu, Y. Xu, J. P. Yanez, S. Yoshida, T. Yuan, Z. Zhang, and M. Zöcklein [hide authors].
The High Altitude Water Cherenkov (HAWC) and IceCube observatories, through
the Astrophysical Multimessenger Observatory Network (AMON) framework, have
developed a multimessenger joint search for extragalactic astrophysical
sources. This analysis looks for sources that emit both cosmic neutrinos and
gamma rays that are produced in photo-hadronic or hadronic interactions. The
AMON system is running continuously, receiving sub-threshold data (i.e. data
that is not suited on its own to do astrophysical searches) from HAWC and
IceCube, and combining them in real-time. We present here the analysis
algorithm, as well as results from archival data collected between June 2015
and August 2018, with a total live-time of 3.0 years. During this period we
found two coincident events that have a false alarm rate (FAR) of $<1$
coincidence per year, consistent with the background expectations. The
real-time implementation of the analysis in the AMON system began on November
20th, 2019, and issues alerts to the community through the Gamma-ray
Coordinates Network with a FAR threshold of $<4$ coincidences per year.
Retrieval of energy spectra for all flavor of neutrinos from
core-collapse supernova with multiple detectors
2008.10082 [abs] [pdf]
[abstract]
by Hiroki Nagakura.
We present a new method by which to retrieve energy spectrum for all flavor
of neutrinos from core-collapse supernova (CCSN). In the retrieval process, we
do not assume any analytic formulae to express the energy spectrum of neutrinos
but rather take a direct way of spectrum reconstruction from the observed data;
the Singular Value Decomposition algorithm with a newly developed adaptive
energy-gridding technique is adopted. We employ three independent reaction
channels having different flavor sensitivity to neutrinos. Two reaction
channels, inverse beta decay on proton and elastic scattering on electrons,
from a water Cherenkov detector such as Super-Kamiokande (SK) and
Hyper-Kamiokande (HK), and a charged current reaction channel with Argon from
the Deep Underground Neutrino Experiment (DUNE) are adopted. Given neutrino
oscillation models, we iteratively search the neutrino energy spectra at the
CCSN source until they provide the consistent event counts in the three
reaction channels. We test the capability of our method by demonstrating the
spectrum retrieval to a theoretical neutrino data compute