bluuebunny/crossref_metadata_2025_split huggingface dataset:
PICOLON dark matter search ˜ Development of highly redio-pure NaI(Tl) scintilltor ˜
Authors: Fushimi Ken-Ichi , Chernyak Dmitry , Ejiri Hiroyasu , Hata Kazumi , Hazama Ryuta , Hirata Shoko , Iida Takashi , Ikeda Haruo , Inoue Kunio , Imagawa Kyoshiro , Kanemitsu Yuta , Kozlov Alexandle , Orito Reiko , Shima Tatsushi , Takemoto Yasuhiro , Umehara Saori , Yoshida Sei 
Published: March 2020

Abstract
The PICOLON project is developing a high purity NaI(Tl) crystal by optimizing the purification methods. The reduction method for 40K was established and we got sufficiently pure NaI(Tl) crystal for 40K. On the other hand, the concentration of 210Pb is still higher than our goal. The investigation is now in progress to fix the origin of the contamination.
The construction of the second phase detector system of PICOLON detector will be started in 2020 spring. The total mass of the second phase is about 54 kg. The background level by the test measurement using a single module is reported.
SaG4n: Calculation of (α,n) yields for low background experiments using Geant4
Authors: Pesudo V , Mendoza E , Alcayne V , Cano-Ott D , Garca-Abia P , Romero L , Romojaro P , Santorelli R 
Published: March 2020

Abstract
SaG4n is a code fully based on Geant4 that we have developed to calculate neutron yields. The code is available in http://win.ciemat.es/SaG4n and works for Geant4.10.6 or superior. The improvements to the (α,n) yields introduced by the use of a single Monte Carlo code, fully developed in Geant4, are presented. Neutrons are a potential source of background for all rare-event searches, and is specially relevant for WIMP searches with liquid argon, where they are the only source of irreducible background together with the yet-negligible coherent neutrino scattering. The precision of the neutron yield is critical to evaluate the discovery potential of coming experiments and to reduce systematic effects in current data.
We present the result of evaluating the neutron yield for three different cases and show the sizable effect of interfaces between materials with high (α,n) cross section and materials with small mass which contribution to the neutron budget is often considered negligible.
Hunting for light dark matter with DUNE PRISM
Authors: Romeri Valentina De , Kelly Kevin J , Machado Pedro A N 
Published: March 2020

Abstract
We present the prospects for exploring low-scale dark sectors with the future DUNE experiment and the impact of the movable off-axis near detector concept, DUNE-PRISM, and a higher energy beam configuration. We focus on a simple scenario which extends the Standard Model by a “dark” U(1), comprising scalar or fermion dark matter and a dark photon kinetically mixed with the photon. We consider nucleus and electron scattering signatures of dark matter produced in the beam via neutral pseudoscalar meson decays. Our results show that, by analysing the energy spectra of single electron events in multiple off-axis angle, DUNE-PRISM can substantially increase the experimental sensitivity to these models, reaching theoretical targets for thermal relic dark matter for a wide range of dark photon and dark matter masses.
The TREX-DM experiment at the Canfranc Underground Laboratory
Authors: Castel J , Cebrián S , Dafni T , Galán J , Irastorza IG , Luzón G , Margalejo C , Mirallas H , Ortiz de Solórzano A , Peiró A , Ruiz-Chóliz E 
Published: March 2020

Abstract
TREX-DM (TPC Rare Event eXperiment for Dark Matter) is intended to look for low mass WIMPs in the Canfranc Underground Laboratory (LSC) in Spain, using light elements (Ne, Ar) as target in a high pressure TPC equipped with Micromegas readouts. Here, a description of the detector, the first results from commissioning data and the expected sensitivity from the developed background model are briefly presented.
Preliminary Design of Pulse Digitalization and Readout Electronics for CDEX-10
Authors: Zhu Jinfu , Xue Tao , Wei Liangjun , Li Jianmin 
Published: March 2020

Abstract
CDEX (China Dark Matter Experiment) is now planning to be upgraded to about 10 Kg HPGe (High Purity Germanium) detectors (CDEX-10) and the new suitable dedicated pulse digitizer and readout electronics are on demand. The readout system is interfaced to the front preamplifiers, which has two “slow” outputs with typical 6-μs shaping time and two “fast” output with typical 300-ns shaping time. In this preliminary design of pulse digitalization and readout electronics, 8-channel 14-Bit 100 MSPS ADC (Analog-to-Digital Converter) and 4-channel 12-Bit 1 GSPS ADC are embedded in the 6U-size readout prototype board. The RAIN1000Z1 readout module based on ZYNQ SoC (System on Chip) is used for readout with Gigabit Ethernet. The ENOB (Effective Number Of Bits) of ADC and the TCP data throughput of Gigabit Ethernet will be discussed. The preliminary result of gamma-ray spectrum will also be presented.
Improved Measurements of the β-Decay Response of Liquid Xenon with the LUX Detector
Authors: Balajthy Jon 
Published: March 2020

Abstract
The LUX experiment was based on a liquid-xenon time-projection chamber that was located on the 4,850’ level of the Sanford Underground Research Facility until it was decommissioned in 2016. In total, the LUX detector contained about 370 kg of xenon, 250 kg of which was active. LUX was designed primarily to detect WIMP dark matter, and produced world-leading limits on the WIMP scattering cross section. In this presentation, I report results from an extensive set of measurements of the β-decay response in liquid xenon. These measurements are derived from high-statistics calibration data from injected sources of both tritium and carbon-14 in the LUX detector after the WIMP-search runs had been completed. The mean light-to-charge ratio is reported for 13 electric field values ranging from 43 to 491 V/cm, and for energies ranging from 1.5 to 145 keV.
Current status and future prospects of the CRAFFT project for the next generation UHECR observatory
Authors: Ikeda Daisuke , Tameda Yuichiro , Tomida Takayuki , Yamazaki Katsuya , Yamamoto Mashu , Iwakura Hirokazu , Nakamura Yuya , Kaino Yuki 
Published: March 2020

Abstract
A key to understand the origin of the Ultra High Energy Cosmic Ray (UHECR) is higher statistics with the composition information. One of the concepts to realize the future huge observation is an array of simple and low cost fluorescence telescopes. The fluorescence telescope can measure not only the arrival direction and energy spectrum but also the mass composition which is the important information to understand the origin of UHECR. A concept of a simple FD is to reduce the cost by changing from the imaging with multiple PMTs to the time information of a few PMTs, and minimization of the optical system by focusing the high energy events. In order to demonstrate this concept, we are developing Cosmic Ray Air Fluorescence Fresnel lens Telescope (CRAFFT), which further reduces the cost by using Fresnel lens and stand alone system without telescope hut unlike existing fluorescence detector in present UHECR observatory. We have constructed four prototype CRAFFTs and observed air showers by simultaneous observation with Telescope Array. By those study, the cost of a simple FD reaches 1/10 of that of a present FD.
A new source type of galactic cosmic rays
Authors: Sinitsyna V.G. , Sinitsyna V.Y. , Stozhkov Yu. I. 
Published: March 2020

Abstract
Experimental data of PAMELA and AMS-02 on proton and helium spectra at high and very high energies as well as the excess of 10 - 300 GeV positron flux cannot be explained using the diffusive models of propagation of cosmic-rays accelerated at the supernova shocks and require the existence of nearby sources of cosmic rays at the distances less than one kpc. We consider active dwarf stars as possible sources of galactic cosmic rays in the energy range up to ˜ 1014 eV. The generation of high-energy cosmic rays should be accompanied by high-energy γ-ray emission, which may be detected. Here we present the SHALON long-term observation data aimed to search for γ-ray emission above 800 GeV from the active red dwarf stars: V962 Tau, V780 Tau, V388 Cas, V1589 Cyg, GJ 1078 and GL 851.1. The TeV gamma-ray emission mostly of aring type from these sources was detected. This result confirms that active dwarf stars are also the sources of high-energy galactic cosmic rays.
Anisotropy of cosmic ray fluxes measured with AMS-02 on the ISS
Authors: Velasco M A , Casaus J , Mañá C , Molero M , Gebauer I , Graziani M , Gervasi M , La Vacca G , Rancoita P G 
Published: March 2020

Abstract
A measurement of the cosmic ray anisotropy on the arrival directions of elementary particles (electrons, positrons and protons) and light nuclei (helium, carbon and oxygen) has been performed in galactic coordinates by the Alpha Magnetic Spectrometer onboard the International Space Station. The analysis is based on the sample of events collected in the first 6.5 years (electrons and positrons), and 7.5 (protons, helium, carbon and oxygen) of data taking. The results are consistent with isotropy for all cosmic ray species and upper limits on the dipole amplitude have been computed. In particular, 95% credible interval upper limits of δ < 1.9% and δ < 0.5% are obtained for positrons and electrons, respectively, above 16 GeV. On the other hand, the upper limits of protons, helium, carbon and oxygen above 200 GV are found to be δ < 0.38%, δ < 0.36%, δ < 1.9% and δ < 1.7%, respectively.
Detection of a γ-ray halo around Geminga with the Fermi-LAT and implications for the positron flux
Authors: Donato Fiorenza , Manconi Silvia , Mauro Mattia Di 
Published: March 2020

Abstract
The HAWC Collaboration has discovered a γ-ray emission extended about 2 degrees around the Geminga and Monogem pulsar wind nebulae (PWNe) at γ-ray energies Eγ
> 5 TeV. We analyze, for the first time, almost 10 years of γ-ray data obtained with the Fermi Large Area Telescope at Eγ
> 8 GeV in the direction of Geminga and Monogem. Since these two pulsars are close the Galactic plane we run our analysis with 10 different interstellar emission models (IEMs) to study the systematics due to the modeling of this component. We detect a γ-ray halo around Geminga with a significance in the range 7.8 − 11.8σ depending on the IEM considered. This measurement is compatible with e+ and e− emitted by the PWN, which inverse-Compton scatter (ICS) with photon fields located within a distance of about 100 pc from the pulsar, where the diffusion coefficient is estimated to be around 1.1 ⋅ 1027 cm2/s at 100 GeV. We include in our analysis the proper motion of the Geminga pulsar which is relevant for γ rays produced for ICS in the Fermi-LAT energy range. We find that an efficiency of about 1% for the conversion of the spin-down energy of the pulsar into e+ and e− is required to be consistent with γ-ray data from Fermi-LAT and HAWC. The inferred contribution of Geminga to the e+ flux is at most 20% at the highest energy AMS-02 data. Our results are compatible with the interpretation that the cumulative emission from Galactic pulsars explains the positron excess.
High-multiplicity muon events observed with EMMA array
Authors: Trzaska Wladyslaw Henryk , Bezrukov Leonid , Enqvist Timo , Inzhechik Lev , Joutsenvaara Jari , Kuusiniemi Pasi , Loo Kai , Lubsandorzhiev Bayarto , Słupecki Maciej 
Published: March 2020

Abstract
High-multiplicity data, collected with a segmented scintillator array of the cosmic-ray experiment EMMA (Experiment with Multi-Muon Array), is presented for the first time. The measurements were done at the depth of 75 meters (210 m.w.e.) in the Pyhäsalmi mine in Finland. EMMA uses two types of detectors: drift chambers and plastic scintillation detectors. The presented data were acquired over the period between December, 2015 and April, 2018 using 128-800 plastic scintillator pixels probing the fiducial area of ˜100 m2. The results are being interpreted in terms of CORSIKA simulations. Several events with densities in excess of 10 muons per m2 were observed. At the next stage of the analysis, the high-multiplicity events will be matched with precision tracking data extracted from the multi-layer drift chambers of EMMA. Observation of high-density muon bundles was first reported by the LEP experiments: DELPHI, L3+C, and ALEPH. More recently, the ALICE experiment at CERN has provided new cosmic-ray results together with improved interpretation benefiting from the updated cross section values extracted from LHC results. While the tracking performance of ALICE is superior to EMMA, the duration of ALICE cosmic-ray measurements is very limited. Over the period of 2010–2018 the total exposure was only 93 days while EMMA, having a similar overburden provides a larger footprint and collects data continuously.
TeV gamma-rays from the region of Perseus Cluster
Authors: Sinitsyna V.G. , Sinitsyna V.Y. 
Published: March 2020

Abstract
The results of 20-year observations of the Perseus cluster centering on the NGC 1275 including IC 310 radio galaxy and extragalactic supernova SN 2006gy at energies 800 GeV - 45 TeV by the SHALON telescope are presented. It was found, that the TeV γ-ray emission at energies > 800 GeV has an extended structure with a distinct core centered at the NGC 1275 nucleus and well correlates with the photon emission regions viewed in X-rays by Chandra and anti-correlates with radio-structures. Also, the variations of TeV γ-ray flux both at year- and day- scales were found. The obtained data indicate that the part of TeV γ-ray emission is generated by relativistic jets in the nucleus of NGC 1275. Whereas, the presence of an extended structure around NGC 1275 and the slow rise of the γ-ray flux is the evidence of the interaction of cosmic rays and magnetic fields generated in the jets at the galactic center with the gas of the Perseus cluster.
Extragalactic background light: Constraints from the TeV gamma-ray observations
Authors: Sinitsyna V.G. , Sinitsyna V.Y. , Borisov S.S. , Balygin K.A. , Klimov A.I. , Mirzafatikhov R.M. , Moseiko N.I. , Ostashev I.E. 
Published: March 2020

Abstract
The cosmological processes including the history of stars and galaxies formation will be observed in the energy spectrum of Extragalactic Background Light (EBL) radiation. Observations of the very high energy γ-ray sources at redshifts from z = 0.018 up to z = 2.979 with SHALON telescopes gives an opportunity to constrain the EBL density, as the TeV γ-rays can be absorbed due to interaction of low-energy photons of EBL. The detection of TeV γ-ray sources at high redshifts is the evidence of less average spectral density of EBL and thus the less star formation rate at early evolution stage as well as the less expansion rate of the universe, than it is previously believed.
Supernova neutrinos in the proto-neutron star cooling phase and nuclear matter
Authors: Nakazato Ken’ichiro , Suzuki Hideyuki 
Published: March 2020

Abstract
A proto-neutron star (PNS) is a newly formed compact object in a core collapse supernova. Using a series of phenomenological equations of state (EOS), we have systematically investigated the neutrino emission from the cooling phase of a PNS. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. As a result, the cooling timescale evaluated from the neutrino light curve is found to be long for the EOS models with small neutron star radius and large effective mass of nucleons. It implies that extracting properties of a PNS (such as mass and radius) and the nuclear EOS is possible by a future supernova neutrino observation.
Turbulence Particle Acceleration and UHECR
Authors: Asano Katsuaki , Teraki Yuto , Hayashida Masaaki , Mészáros Peter 
Published: March 2020

Abstract
The standard model to produce non-thermal particles is the particle acceleration at shocks. However, the photon spectra in high-energy objects, such as blazars, frequently show very hard feature, which seems inconsistent with the standard shock acceleration theory. The alternative model is the particle acceleration by turbulence. If we adopt a hard-sphere-like acceleration, in which the acceleration timescale is independent of the particle energy, the electron energy distribution becomes consistent with blazar photon spectra. Adopting this model to the deceleration phase of gamma-ray burst jets, ultra high-energy cosmic-rays can be produced. The resultant spectrum is harder than other models, so that the secondary neutrino production in their propagation is relatively suppressed. As a candidate of the hard-sphere acceleration mechanism, we propose the acceleration by large scale compressible MHD waves, where the transit time damping (TTD) is a key mechanism. We find that the acceleration efficiency is higher than previously considered.
Neutrinos from blazars
Authors: Cerruti Matteo 
Published: March 2020

Abstract
The evidence for joint gamma and neutrino emission from the blazar TXS 0506+056 has renewed interest in blazars as neutrino sources. The detection of neutrinos from blazars can be seen as the smoking gun for the presence of relativistic protons in blazar’s jets, and can thus help identify blazars, and active galactic nuclei in general, as cosmic-ray accelerators. In this contribution I first introduce blazars and blazar hadronic models, and then present the results of the multi-messenger modeling of both the 2017 gamma-neutrino flare, and the 2014-2015 neutrino-only flare of TXS 0506+056. For the first time it is possible to constrain blazar hadronic models using the information from neutrino detectors, and I discuss the implications of these neutrino observations on our understanding of the physics of relativistic jets from super-massive black-holes.
NICHE detector and operations
Authors: Omura Yugo , Bergman Douglas R , Krizmanic John F , Nakai Kei , Tsunesada Yoshiki 
Published: March 2020

Abstract
The Non-Imaging CHErenkov Array (NICHE) is a low energy extension to Telescope Array and TALE using an array of closely spaced (˜ 200m) light collectors covering an area of ˜ 2 square km. It is being deployed in the field of view of TALE and will overlap it in the energy range above 4 PeV. Cosmic ray air showers with energies 1-100 PeV are reconstructed using both the Cherenkov light Lateral Distribution and the Cherenkov time Width Lateral Distribution. These two methods will allow shower energy and X
max to be determined. A prototype of the array, called j-NICHE, has been deployed. The performance of detector’s components, current status of the detectors and the observations are presented.
Neutrino distributions for a rotating core-collapse supernova with a Boltzmann-neutrino-transport
Authors: Harada Akira 
Published: March 2020

Abstract
We simulate the collapse of a rotating core of the progenitor with 11.2 solar mass with the Boltzmann-radiation-hydrodynamics code, which solves the Boltzmann equations for neutrino transfer directly. We pay particular attention to the neutrino distribution in phase space, which is affected by the rotation. By solving the Boltzmann equations directly, we can assess the rotation-induced distortion of the angular distribution in momentum space, which gives rise to the rotational component of the neutrino flux. We compare the Eddington tensors calculated both from the raw data and from the M1-closure approximation. We find that the difference in the Eddington factors reaches ˜ 20% in our simulation. This is due to the different dependence of the Eddington and flux factors on the angular profile of the neutrino distribution function, and hence modification to the closure relation is needed.
Can the TeV gamma-ray sky probe the galactic cosmic ray distribution?
Authors: Pagliaroli G. , Cataldo M. , Vecchiotti V. , Villante F.L. 
Published: March 2020

Abstract
We evaluate the diffuse gamma-ray flux at TeV energies produced by hadronic interactions of cosmic rays with the gas contained in the galactic disk. We consider different assumptions for the cosmic ray distribution, including the recently emerged possibility of a harder cosmic ray spectrum in the inner Galaxy. We show that observational data provided by Argo-YBJ, HESS, HAWC and Milagro, can already discriminate among different hyphoteses. The constraints can be strengthened if the contribution of sources not resolved by HESS is taken into account.
Variations of cosmic ray muon flux during thunderstorms as a tool for studying electric field distribution and particle production processes in the atmosphere
Authors: Khaerdinov M N , Khaerdinov N S , Lidvansky A S 
Published: March 2020

Abstract
The recently published result of GRAPES-3 (a strong thunderstorm muon intensity change) and conclusions made on its basis by this collaboration are discussed and compared with the Baksan observations of muon variations during thunderstorms performed much earlier. It is demonstrated that generally both experiments are quite consistent as far as characteristic patterns of events are concerned, as well as conclusions about direct connection between amplitude of muon intensity disturbance and electric field strength in the atmosphere. However, the GRAPES-3 conclusion about gigavolt potentials associated with their event is doubtful and seems to contradict the fundamental limits on electric fields that can exist in the atmosphere.
Search for cosmic gamma rays of ultra-high energies with the Baksan air shower array
Authors: Lidvansky A S , Dzhappuev D D , Petkov V B , Gorbacheva E A , Dzaparova I M , Kudzhaev A U , Klimenko N F , Kurenya A N , Mikhailova O I , Romanenko V S , Khadziev M M , Yanin A F 
Published: March 2020

Abstract
Recently two collaborations (Tibet ASγ and HAWC) almost simultaneously reported about their measurements of ultra-high-energy (> 100 TeV) gamma rays from the Crab Nebula. The Baksan air shower array (BASA) recorded a burst from this very source as long ago as more than 20 years. At the moment the new experiment on gamma ray astronomy (Carpet-3 project) started at Baksan, and it is appropriate to recall old results of BASA to be compared with the new results, already published and expected.
Effect of shadowing and antishadowing corrections to the evolution of gluon density at small-x
Authors: Devee Mayuri 
Published: March 2020

Abstract
We have obtained a semi-analytical solution of GLR-MQ-ZRS equation at small x for gluon density using Regge like ansatz of G(x,Q
2) in the leading twist approximation. It is observed that, our solution is valid in the vicinity of saturation scale where modification in the QCD evolution can not be ruled out due to salient gluon fusion processes. Our computed results of nonlinear gluon density are then compared with different global parameterizations and it is enticing to note that, the rapid growth of gluon densities towards small-x is tamed due to the nonlinear corrections.
Search for triple and quadruple beta decay of 150Nd using low-background HPGe detector
Authors: Barabash A.S. , Hubert Ph. , Nachab A. , Umatov V.I. 
Published: March 2020

Abstract
Triple beta decay of 150Nd to the ground and excited states of 150Eu and quadruple beta decay of 150Nd to the excited states of 150Gd have been studied using a 400 cm3 low-background HPGe detector. A half-life limit for the quadruple beta decay to the

0
1
+

state of 150Gd was found to be T1/2(0v + 4v) > 8.7 × 1020 yr (90% C.L.). For other (0v+4v) transitions to the excited states limits for the first time have been obtained at the level of (6.1 − 9.5) × 1020 yr (90% C.L.). We report here also the results for the first search for triple beta decay to the ground and excited final states of 150Eu, T
1/2(0v + 3v) > (0.04 − 4.8) × 1020 yr (90% C.L.).