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arXiv 2025年

作者： Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Argüelles, C. Ashida, Y. Athanasiadou, S. Axani, S.N. Babu, R. Bai, X. Balagopal, V.A. Baricevic, M. Barwick, S.W. Bash, S. Basu, V. Bay, R. Beatty, J.J. Tjus, J. Becker Beise, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Blaufuss, E. Bloom, L. Blot, S. Bontempo, F. Motzkin, J.Y. Book Meneguolo, C. Boscolo Böser, S. Botner, O. Böttcher, J. Braun, J. Brinson, B. Brisson-Tsavoussis, Z. Brostean-Kaiser, J. Brusa, L. Burley, R.T. Butterfield, D. Campana, M.A. Caracas, I. Carloni, K. Carpio, J. Chattopadhyay, S. Chau, N. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Coleman, A. Coleman, P. Collin, G.H. Connolly, A. Conrad, J.M. Corley, R. Cowen, D.F. De Clercq, C. DeLaunay, J.J. Delgado, D. Deng, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dierichs, P. Dittmer, M. Domi, A. Draper, L. Dujmovic, H. Durnford, D. Dutta, K. DuVernois, M.A. Ehrhardt, T. Eidenschink, L. Eimer, A. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. Esmail, W. Evans, J. Evenson, P.A. Fan, K.L. Fang, K. Farrag, K. Fazely, A.R. Fedynitch, A. Feigl, N. Fiedlschuster, S. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Fukami, S. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Garcia, M. Garg, G. Genton, E. Gerhardt, L. Ghadimi, A. Girard-Carillo, C. Glaser, C. Glüsenkamp, T. Gonzalez, J.G. Goswami, S. Granados, A. Grant, D. Gray, S.J. Griffin, S. Griswold, S. Groth, K.M. Guevel, D. Günther, C. Gutjahr, P. Ha, C. Haack, C. Hallgren, A. Halve, L. Halzen, F. Hamacher, L. Hamdaoui, H. Minh, M. Ha Handt, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haungs, A. Häußler, J. Helbing, K. Hellrung, J. Hermannsgabner, J. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hill, C. Hill, G.C. Hmaid, R. Hoffman, K.D. Hori, S. Hoshina, K. Hostert, M. III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Dept. of Physics Simon Fraser University BurnabyBCV5A 1S6 Canada Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics The International Center for Hadron Astrophysics Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute University of Copenhagen CopenhagenDK-2100 Denmark Dept. of Physics TU Dortmund University DortmundD-44221 Germany Dept. of Physics and

We report a measurement of the inelasticity distribution in the scattering of neutrinos of energy 80−560 GeV off nucleons, which is sensitive to the inclusive differential cross section. This analysis is based on a sample of atmospheric muon neutrinos detected in the IceCube sub-array DeepCore during 2012-2021, and is the first such measurement in this energy range. Our measurement extends to energies where accelerator data is not available, hence we compare our results to predictions from perturbative QCD calculations, finding good agreement. Copyright © 2025, The Authors. All rights reserved.

关键词： Neutrons

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Dealing with density discontinuities in planetary SPH simulations

arXiv

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arXiv 2022年

作者： Ruiz-Bonilla, S. Borrow, J. Eke, V.R. Kegerreis, J.A. Massey, R.J. Sandnes, T.D. Teodoro, L.F.A. Institute for Computational Cosmology Durham University South Road DurhamDH1 3LE United Kingdom Institute for Data Science Durham University South Road DurhamDH1 3LE United Kingdom Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States NASA Ames Research Center Moffett Field CA United States BAERI NASA Ames Research Center Moffett Field CA United States School of Physics and Astronomy University of Glasgow G12 8QQ United Kingdom

Density discontinuities cannot be precisely modelled in standard formulations of smoothed particles hydrodynamics (SPH) because the density field is defined smoothly as a kernel-weighted sum of neighbouring particle masses. This is a problem when performing simulations of giant impacts between proto-planets, for example, because planets typically do have density discontinuities both at their surfaces and at any internal boundaries between different materials. The inappropriate densities in these regions create artificial forces that effectively suppress mixing between particles of different material and, as a consequence, this problem introduces a key unknown systematic error into studies that rely on SPH simulations. In this work we present a novel, computationally cheap method that deals simultaneously with both of these types of density discontinuity in SPH simulations. We perform standard hydrodynamical tests and several example giant impact simulations, and compare the results with standard SPH. In a simulated Moon-forming impact using 107 particles, the improved treatment at boundaries affects at least 30% of the particles at some point during the simulation. © 2022, CC BY.

关键词： Hydrodynamics

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Performance of the D-Egg Optical Sensor for the IceCube Upgrade 37

Performance of the D-Egg Optical Sensor for the IceCube Upgr...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Hill, Colton Meier, Maximillian Nagai, Ryo Kin, Ken’ichi Shimizu, Nobuhiro Ishihara, Aya Yoshida, Shigeru Anderson, Tyler Braun, Jim Fienberg, Aaron Weber, Jeff Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Blaufuss, E. Blot, S. Boddenberg, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. De Clercq, C. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haungs, A. Hauser, S. Hebecker, D. Helbing, K. Henningsen, F. Hettinger, E.C. Hickford, S. Hignight, J. Dept. of Physics Institute for Global Prominent Research Chiba University Japan Dept. of Astronomy and Astrophysics Pennsylvania State University University Park United States Dept. of Physics Wisconsin IceCube Particle Astrophysics Center University of Wisconsin Madison United States III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics Institute for Global Prominent Research Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. o

New optical sensors called the "D-Egg" have been developed for cost-effective instrumentation for the IceCube Upgrade. With two 8-inch high quantum efficient photomultiplier tubes (PMTs), they offer increased effective photocathode area while retaining as much of the successful IceCube Digital Optical Module design as possible. Mass production of D-Eggs has started in 2020. By the end of 2021, there will be 310 D-Eggs produced with 288 deployed in the IceCube Upgrade. The D-Egg readout system uses advanced technologies in electronics and computing power. Each of the two PMT signals is digitised using ultra-low-power 14-bit ADCs with a sampling frequency of 240 MSPS, enabling seamless and lossless event recording from single-photon signals to signals exceeding 200 PE within 10 ns, as well as flexible event triggering. In this paper, we report the single photon detection performance as well as the multiple photon recording capability of D-Eggs from the mass production line which have been evaluated with the built-in data acquisition system. © Copyright owned by the author(s).

关键词： Photomultipliers

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Search for neutrino lines from dark matter annihilation and decay with IceCube

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Physical Review D 2023年第10期108卷 102004-102004页

作者： R. Abbasi M. Ackermann J. Adams S. K. Agarwalla J. A. Aguilar M. Ahlers J. M. Alameddine N. M. Amin K. Andeen G. Anton C. Argüelles Y. Ashida S. Athanasiadou S. N. Axani X. Bai A. Balagopal M. Baricevic S. W. Barwick V. Basu S. Baur R. Bay J. J. Beatty K.-H. Becker J. Becker Tjus J. Beise C. Bellenghi S. BenZvi D. Berley E. Bernardini D. Z. Besson G. Binder D. Bindig E. Blaufuss S. Blot F. Bontempo J. Y. Book C. Boscolo Meneguolo S. Böser O. Botner J. Böttcher E. Bourbeau J. Braun B. Brinson J. Brostean-Kaiser R. T. Burley R. S. Busse D. Butterfield M. A. Campana K. Carloni E. G. Carnie-Bronca S. Chattopadhyay N. Chau C. Chen Z. Chen D. Chirkin S. 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 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 A. Domi H. Dujmovic M. A. DuVernois T. Ehrhardt C. El Aisati P. Eller R. Engel H. Erpenbeck J. Evans P. A. Evenson K. L. Fan K. Fang A. R. Fazely A. Fedynitch N. Feigl S. Fiedlschuster C. Finley L. Fischer D. Fox A. Franckowiak E. Friedman A. Fritz P. Fürst T. K. Gaisser J. Gallagher E. Ganster A. Garcia L. Gerhardt A. Ghadimi C. Glaser T. Glauch T. Glüsenkamp N. Goehlke J. G. Gonzalez S. Goswami D. Grant S. J. Gray S. Griffin S. Griswold C. Günther M. Gustafsson P. Gutjahr C. Haack A. Hallgren R. Halliday L. Halve F. Halzen T. Hambye H. Hamdaoui M. Ha Minh K. Hanson J. Hardin A. A. Harnisch P. Hatch A. Haungs K. Helbing J. Hellrung F. Henningsen L. Heuermann N. Heyer 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 A. Ishihara M. Jacquart M. Jansson G. S. Japaridze K. Jayakumar 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. Khatee Zathul A. Kheirandish J. Kiryluk S. R. Klein A. Kochocki R. Koiral Department of Physics Loyola University Chicago Chicago Illinois 60660 USA Deutsches Elektronen-Synchrotron DESY Platanenallee 6 15738 Zeuthen Germany Department of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Department of Physics and Wisconsin IceCube Particle Astrophysics Center University of Wisconsin–Madison Madison Wisconsin 53706 USA Université Libre de Bruxelles Science Faculty CP230 B-1050 Brussels Belgium Niels Bohr Institute University of Copenhagen DK-2100 Copenhagen Denmark Department of Physics TU Dortmund University D-44221 Dortmund Germany Bartol Research Institute and Department of Physics and Astronomy University of Delaware Newark Delaware 19716 USA Department of Physics Marquette University Milwaukee Wisconsin 53201 USA Erlangen Centre for Astroparticle Physics Friedrich-Alexander-Universität Erlangen-Nürnberg D-91058 Erlangen Germany Department of Physics and Laboratory for Particle Physics and Cosmology Harvard University Cambridge Massachusetts 02138 USA Physics Department South Dakota School of Mines and Technology Rapid City South Dakota 57701 USA Department of Physics and Astronomy University of California Irvine California 92697 USA Department of Physics University of California Berkeley California 94720 USA Department of Astronomy Ohio State University Columbus Ohio 43210 USA Department of Physics and Center for Cosmology and Astro-Particle Physics Ohio State University Columbus Ohio 43210 USA Department of Physics University of Wuppertal D-42119 Wuppertal Germany Fakultät für Physik and Astronomie Ruhr-Universität Bochum D-44780 Bochum Germany Department of Physics and Astronomy Uppsala University Box 516 S-75120 Uppsala Sweden Physik-department Technische Universität München D-85748 Garching Germany Department of Physics and Astronomy University of Rochester Rochester New York 14627 USA Department of Physics University of Maryland College Park Maryland 20742 US

Dark matter particles in the Galactic center and halo can annihilate or decay into a pair of neutrinos producing a monochromatic flux of neutrinos. The spectral feature of this signal is unique and it is not expected from any astrophysical production mechanism. Its observation would constitute a dark matter smoking gun signal. We performed the first dedicated search with a neutrino telescope for such signal, by looking at both the angular and energy information of the neutrino events. To this end, a total of five years of IceCube’s DeepCore data has been used to test dark matter masses ranging from 10 GeV to 40 TeV. No significant neutrino excess was found and upper limits on the annihilation cross section, as well as lower limits on the dark matter lifetime, were set. The limits reached are of the order of 10−24 cm3/s for an annihilation and up to 1027 s for decaying dark matter. Using the same data sample we also derive limits for dark matter annihilation or decay into a pair of Standard Model charged particles.

关键词： particle astrophysics particle dark matter Weakly interacting massive particles Cosmic ray & astroparticle detectors Neutrino detection

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Search for electron-antineutrinos associated with gravitational-wave events GW150914,GW151012,GW151226,GW170104,GW170608,GW170814,and GW170817 at Daya Bay

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Chinese physics C 2021年第5期45卷 190-201页

作者： F.P.An A.B.Balantekin H.R.Band M.Bishai S.Blyth G.F.Cao J.Cao J.F.Chang Y.Chang H.S.Chen S.M.Chen Y.Chen Y.X.Chen J.Cheng Z.K.Cheng J.J.Cherwinka M.C.Chu J.P.Cummings O.Dalager F.S.Deng Y.Y.Ding M.V.Diwan T.Dohnal J.Dove M.Dvorak D.A.Dwyer J.P.Gallo M.Gonchar G.H.Gong H.Gong W.Q.Gu J.Y.Guo L.Guo X.H.Guo Y.H.Guo Z.Guo R.W.Hackenburg S.Hans M.He K.M.Heeger Y.K.Heng A.Higuera Y.K.Hor Y.B.Hsiung B.Z.Hu J.R.Hu T.Hu Z.J.Hu H.X.Huang X.T.Huang Y.B.Huang P.Huber D.E.Jaffe K.L.Jen X.L.Ji X.P.Ji R.A.Johnson D.Jones L.Kang S.H.Kettell S.Kohn M.Kramer T.J.Langford J.Lee J.H.C.Lee R.T.Lei R.Leitner J.K.C.Leung F.Li J.J.Li Q.J.Li S.Li S.C.Li W.D.Li X.N.Li X.Q.Li Y.F.Li Z.B.Li H.Liang C.J.Lin G.L.Lin S.Lin J.J.Ling J.M.Link L.Littenberg B.R.Littlejohn J.C.Liu J.L.Liu C.Lu H.Q.Lu J.S.Lu K.B.Luk X.B.Ma X.Y.Ma Y.Q.Ma C.Marshall D.A.Martinez Caicedo K.T.MeDonald R.D.McKeown Y.Meng J.Napolitano D.Naumov E.Naumova J.P.Ochoa-Ricoux A.OIshevskiy H.-R.Pan J.Park S.Patton J.C.Peng C.S.J.Pun F.Z.Qi M.Qi X.Qian N.Raper J.Ren C.Morales Reveco R.Rosero B.Roskovec X.C.Ruan H.Steiner J.L.Sun T.Tmej K.Treskov W.-H.Tse C.E.Tull B.Viren V.Vorobel C.H.Wang J.Wang M.Wang N.Y.Wang R.G.Wang W.Wang W.Wang X.Wang Y.Wang Y.F.Wang Z.Wang Z.Wang Z.M.Wang H.Y.Wei L.H.Wei L.J.Wen K.Whisnant C.G.White H.L.H.Wong E.Worcester D.R.Wu F.L.Wu Q.Wu W.J.Wu D.M.Xia Z.Q.Xie Z.Z.Xing J.L.Xu T.Xu T.Xue C.G.Yang L.Yang Y.Z.Yang H.F.Yao M.Ye M.Yeh B.L.Young H.Z.Yu Z.Y.Yu B.B.Yue S.Zeng Y.Zeng L.Zhan C.Zhang F.Y.Zhang H.H.Zhang J.W.Zhang Q.M.Zhang X.T.Zhang Y.M.Zhang Y.X.Zhang Y.Y.Zhang Z.J.Zhang Z.P.Zhang Z.Y.Zhang J.Zhao L.Zhou H.L.Zhuang J.H.Zou Instiute of Modern Physics East China University of Science and TechnologyShanghai 200237 University of Wisconsin MadisonWisconsin 53706 Wright Laboratory and Department of Physics Yale UniversityNew HavenConnecticut 06520 Brookhaven National Laboratory UptonNew York 11973 Department of Physics National Taiwan UniversityTaipei Institute of High Energy Physics Beijing 100049 National United University Miao-Li Department of Engineering Physics Tsinghua UniversityBejing 100084 Shenzhen University Shenzhen 518060 Sun Yat-Sen(Zhongshan)University Guangzhou North China Electric Power University Bejjing 102206 Chinese University of Hong Kong Hong Kong 999077 Siena College LoudonvilleNew York 12211 Department of Physics and Astronomy University of CaliforniaIrvineCaliformia 92697 University of Science and Technology of China Hefei 230026 Charles University Faculty of Mathematics and PhysicsPrague Department of Physics University of llinois at Urbana-ChampaignUrbanaIlinois 61801 Lawrence Berkeley National Laboratory BerkeleyCalifornia 94720 Department of Physics Illinois Institute of TechnologyChicagoIllinois 60616 Joint Institute for Nuclear Research DubnaMoscow Region Beijing Normal University Beijing 100875 Department of Nuclear Science and Technology School of Energy and Power EngineeringXi'an Jiaotong UniversityXi'an 710049 Department of Physics University of HoustonHoustonTexas 77204 China Institute of Atomic Energy Beijing 102413 Shandong University Jinan 250100 Guangxi University Nanning 530004 Center for Neutrino Physics Virginia TechBlacksburgVirginia 24061 Institute of Physics National Chiao-Tung UniversityHsinchu Department of Physics University of CincinnatiCincinnatiOhio 45221 Department of Physies Collge of Science and TechnologyTemple UniversityPhiladelphiaPennsylvania 19122 Dongguan University of Technology Dongguan 523808 Department of Physics University of CaliforniaBerkeleyCalifornia 94720 Department of Physics The University of Hong KongPokfulamHong Kong 999077 School

The establishment of a possible connection between neutrino emission and gravitational-wave(GW)bursts is important to our understanding of the physical processes that occur when black holes or neutron stars *** the Daya Bay experiment,using the data collected from December 2011 to August 2017,a search was per-formed for electron-antineutrino signals that coincided with detected GW events,including GW150914,GW151012,GW151226,GW170104,GW170608,GW 170814,and GW *** used three time windows of±10,±500,and±1000 s relative to the occurrence of the GW events and a neutrino energy range of 1.8 to 100 MeV to search for correlated neutrino *** detected electron-antineutrino candidates were consistent with the expected background rates for all the three time *** monochromatic spectra,we found upper limits(90%confidence level)of the electron-antineutrino fluence of(1.13-2.44)×10^(11)cm^(-2)at 5 MeV to 8.0×10^(7)cm^(-2)at 100 MeV for the three time w *** the assumption of a Fermi-Dirac spectrum,the upper limits were found to be(5.4-7.0)×10^(9)cm^(2)for the three time windows.

关键词： grav itational waves electron-antineutrinos fluence upper limit

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A calibration study of local ice and optical sensor properties in IceCube 37

A calibration study of local ice and optical sensor properti...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Chirkin, Dmitry Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Blaufuss, E. Blot, S. Boddenberg, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. De Clercq, C. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haungs, A. Hauser, S. Hebecker, D. Helbing, K. Henningsen, F. Hettinger, E.C. Hickford, S. Hignight, J. Hill, C. Hill, G.C. Hoffman, K.D. Hoffmann, R. Hoinka, T. Hokanson-Fasig, B. Hoshina, K. Huang, F. Huber, M. Huber, T. Hultqvist, K. Hünnefeld, M. Hussain, R. In, S. Iovine, N. Ishihara, A. Dept. of Physics Wisconsin IceCube Particle Astrophysics Center University of Wisconsin MadisonWI53706 United States III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics Institute for Global Prominent Research Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute University of Copenhagen Copenhage

The optical sensors of the IceCube Neutrino Observatory are attached on vertical strings of cables. They were frozen into the ice in the deployment holes made by hot water drill. This hole ice, to the best of our knowledge, consists of a bubbly central column, with the remainder of the re-frozen volume being optically clear. The bubbly ice often blocks one or several of the calibration LEDs in every optical sensor and significantly distorts the angular profile of the calibration light pulses. It also affects the sensors’ response to in-coming photons at different locations and directions. We present our modeling of the hole ice optical properties as well as optical sensor location and orientation within the hole ice. The shadowing effects of cable string and possible optical sensor tilt away from the nominal vertical alignment are also discussed. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Ice

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UHECR mass composition from anisotropy of their arrival directions with the Telescope Array SD 37

UHECR mass composition from anisotropy of their arrival dire...

引用

37th International Cosmic Ray Conference, ICRC 2021

作者： Kuznetsov, Mikhail Tinyakov, Peter Abbasi, R.U. Abu-Zayyad, T. Allen, M. Arai, Y. Arimura, R. Barcikowski, E. Belz, J.W. Bergman, D.R. Blake, S.A. Buckland, I. Cady, R. Cheon, B.G. Chiba, J. Chikawa, M. Fujii, T. Fujisue, K. Fujita, K. Fujiwara, R. Fukushima, M. Fukushima, R. Furlich, G. Gonzalez, R. Hanlon, W. Hayashi, M. Hayashida, N. Hibino, K. Higuchi, R. Honda, K. Ikeda, D. Inadomi, T. Inoue, N. Ishii, T. Ito, H. Ivanov, D. Iwakura, H. Iwasaki, A. Jeong, H.M. Jeong, S. Jui, C.C.H. Kadota, K. Kakimoto, F. Kalashev, O. Kasahara, K. Kasami, S. Kawai, H. Kawakami, S. Kawana, S. Kawata, K. Kharuk, I. Kido, E. Kim, H.B. Kim, J.H. Kim, M.H. Kim, S.W. Kimura, Y. Kishigami, S. Kubota, Y. Kurisu, S. Kuzmin, V. Kuznetsov, M. Kwon, Y.J. Lee, K.H. Lubsandorzhiev, B. Lundquist, J.P. Machida, K. Matsumiya, H. Matsuyama, T. Matthews, J.N. Mayta, R. Minamino, M. Mukai, K. Myers, I. Nagataki, S. Nakai, K. Nakamura, R. Nakamura, T. Nakamura, T. Nakamura, Y. Nakazawa, A. Nishio, E. Nonaka, T. Oda, H. Ogio, S. Ohnishi, M. Ohoka, H. Oku, Y. Okuda, T. Omura, Y. Ono, M. Onogi, R. Oshima, A. Ozawa, S. Park, I.H. Potts, M. Pshirkov, M.S. Remington, J. Rodriguez, D.C. Rubtsov, G.I. Ryu, D. Sagawa, H. Sahara, R. Saito, Y. Sakaki, N. Sako, T. Sakurai, N. Sano, K. Sato, K. Seki, T. Sekino, K. Shah, P.D. Shibasaki, Y. Shibata, F. Shibata, N. Shibata, T. Shimodaira, H. Shin, B.K. Shin, H.S. Shinto, D. Smith, J.D. Sokolsky, P. Sone, N. Stokes, B.T. Stroman, T.A. Takagi, Y. Takahashi, Y. Takamura, M. Takeda, M. Takeishi, R. Taketa, A. Takita, M. Tameda, Y. Tanaka, H. Tanaka, K. Tanaka, M. Tanoue, Y. Thomas, S.B. Thomson, G.B. Tinyakov, P. Tkachev, I. Tokuno, H. Tomida, T. Troitsky, S. Tsuda, R. Tsunesada, Y. Uchihori, Y. Udo, S. Uehama, T. Urban, F. Wong, T. Yada, K. Yamamoto, M. Yamazaki, K. Yang, J. Yashiro, K. Yoshida, F. Yoshioka, Y. Zhezher, Y. Zundel, Z. Service de Physique Theorique Universite Libre de Bruxelles Boulevard du Triomphe CP225 Brussels1050 Belgium Institute for Nuclear Research of the Russian Academy of Sciences 60th October Anniversary Prospect 7a Moscow117312 Russia Department of Physics Loyola University Chicago ChicagoIL United States The Graduate School of Science and Engineering Saitama University Saitama Saitama Japan High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT United States Graduate School of Science Osaka City University Osaka Osaka Japan Department of Physics The Research Institute of Natural Science Hanyang University Seongdong-gu Seoul Korea Republic of Department of Physics Tokyo University of Science Chiba Noda Japan Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa Japan The Hakubi Center for Advanced Research Graduate School of Science Kyoto University Kitashirakawa-Oiwakecho Sakyo-ku Kyoto Japan Todai Institutes for Advanced Study University of Tokyo Chiba Kashiwa Japan Information Engineering Graduate School of Science and Technology Shinshu University Nagano Nagano Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama Japan Interdisciplinary Graduate School of Medicine and Engineering University of Yamanashi Yamanashi Kofu Japan Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano Japan Astrophysical Big Bang Laboratory RIKEN Saitama Wako Japan Department of Physics Sungkyunkwan University Jang-an-gu Suwon Korea Republic of Department of Physics Tokyo City University Setagaya-ku Tokyo Japan Institute for Nuclear Research of the Russian Academy of Sciences Moscow Russia Faculty of Systems Engineering and Science Shibaura Institute of Technology Minato-ku Tokyo Japan Department of Engineering Science Faculty of Engineering Osaka Electro-Communication University Neyagawa-shi Osaka Japan Departmen

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 modeled with a flux-weighed 2MRS catalog. 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. We apply the method to Telescope Array surface detector data for 11 years and derive new independent constraints on fraction of protons and iron in p-Fe mix at E > 10 EeV. At 10 100 EeV — pure iron or even more massive composition. This result is in tension with Auger composition model inferred from spectrum–Xmax fit at 2.7σ (2.0σ) for PT’11 (JF’12) regular GMF model. © Copyright owned by the author(s).

关键词： Iron

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Antineutrino energy spectrum unfolding based on the Daya Bay measurement and its applications

引用

Chinese physics C 2021年第7期45卷 1-19页

作者： F.P.An A.B.Balantekin M.Bishai S.Blyth G.F.Cao J.Cao J.F.Chang Y.Chang H.S.Chen S.M.Chen Y.Chen Y.X.Chen J.Cheng Z.K.Cheng J.J.Cherwinka M.C.Chu J.P.Cummings O.Dalager F.S.Deng Y.Y.Ding M.V.Diwan T.Dohnal D.Dolzhikov J.Dove M.Dvorak D.A.Dwyer J.P.Gallo M.Gonchar G.H.Gong H.Gong M.Grassi W.Q.Gu J.Y.Guo L.Guo X.H.Guo Y.H.Guo Z.Guo R.W.Hackenburg S.Hans a M.He K.M.Heeger Y.K.Heng Y.K.Hor Y.B.Hsiung B.Z.Hu J.R.Hu T.Hu Z.J.Hu H.X.Huang J.H.Huang X.T.Huang Y.B.Huang P.Huber D.E.Jaffe K.L.Jen X.L.Ji X.P.Ji R.A.Johnson D.Jones L.Kang S.H.Kettel S.Kohn M.Kramer T.J.Langford J.Lee J.H.C.Lee R.T.Lei R.Leitner J.K.C.Leung F.Li H.L.Li J.J.Li Q.J.Li R.H.Li S.Li S.C.Li W.D.Li X.N.Li X.Q.Li Y.F.Li Z.B.Li H.Liang C.J.Lin G.L.Lin S.Lin J.J.Ling J.M.Link26 L.Littenberg B.R.Littlejohn J.C.Liu J.L.Liu J.X.Liu C.Lu H.Q.Lu K.B.Luk B.Z.Ma X.B.Ma X.Y.Ma Y.Q.Ma R.C.Mandujano C.Marshall K.T.McDonald R.D.McKeown Y.Meng J.Napolitano D.Naumov E.Naumova T.M.T.Nguyen J.P.Ochoa-Ricoux A.Olshevskiy H.-R.Pan J.Park S.Patton J.C.Peng C.S.J.Pun F.Z.Qi M.Qi X.Qian N.Raper J.Ren C.Morales Reveco R.Rosero B.Roskovec X.C.Ruan H.Steiner J.L.Sun T.Tmej1 K.Treskov W.-H.Tse C.E.Tull B.Viren V.Vorobel C.H.Wang J.Wang M.Wang N.Y.Wang R.G.Wang W.Wang W.Wang X.Wang Y.Wang Y.F.Wang Z.Wang Z.Wang Z.M.Wang H.Y.Wei L.H.Wei L.J.Wen K.Whisnant C.G.White H.L.H.Wong E.Worcester D.R.Wu F.L.Wu Q.Wu W.J.Wu D.M.Xia Z.Q.Xie Z.Z.Xing H.K.Xu J.L.Xu T.Xu T.Xue C.G.Yang L.Yang Y.Z.Yang H.F.Yao M.Ye M.Yeh B.L.Young H.Z.Yu Z.Y.Yu B.B.Yue V.Zavadskyi S.Zeng Y.Zeng L.Zhan C.Zhang F.Y.Zhang H.H.Zhang J.W.Zhang Q.M.Zhang S.Q.Zhang X.T.Zhang Y.M.Zhang Y.X.Zhang Y.Y.Zhang Z.J.Zhang Z.P.Zhang Z.Y.Zhang J.Zhao R.Z.Zhao L.Zhou H.L.Zhuang J.H.Zou Institute of Modern Physics East China University of Science and TechnologyShanghai 200337 University of Wisconsin MadisonWisconsin 53706 Brookhaven National Laboratory UptonNew York 11973 Department of Physics Nnational Taiwan UniversityTaipei Institute of High Energy Physics Beijing 100049 National United University Miao-Li Department of Engineering Physics Tsinghua UniversityBeijing 100048 Shenzhen University Shenzhen 518061 Sun Yat-Sen(Zhongshan)University Guangzhou 510275 North China Electric Power University Beijing 102206 Chinese University of Hong Kong Hongkong 999077 Siena College LoudonvilleNew York 12211 Department of Physics and Astronomy University of CaliforniaIrvineCalifornia 92697 University of Science and Technology of China Hefei 230022 Charles University Faculty of Mathematics and PhysicsPrague Joint Institute for Nuclear Research DubnaMoscow Region Department of Physics University of Illinois at Urbana-ChampaignUrbanaIllinois 61801 Lawrence Berkeley National Laboratory BerkeleyCalifornia 94720 Department of Physics Illinois Institute of TechnologyChicagoIllinois 60616 Beijing Normal University Beijing 100875 Department of Nuclear Science and Technology School of Energy and Power EngineeringXi'an Jiaotong UniversityXi'an 710049 Wright Laboratory and Department of Physics Yale UniversityNew HavenConnecticut 06520 China Institute of Atomic Energy Beijing 102413 Shandong University Jinan 250002 Guangxi University No.100 Daxue East RoadNanning 530004 Center for Neutrino Physics Virginia TechBlacksburgVirginia 24061 Institute of Physics NCTUHsinchu Department of Physics University of CincinnatiCincinnatiOhio 45221 Department of Physics College of Science and TechnologyTemple UniversityPhiladelphiaPennsylvania 19122 Dongguan University of Technology Dongguan 523808 Department of Physics University of CaliforniaBerkeleyCalifornia 94720 Department of Physics The University of Hong KongPokfulamHongkong 999077 School of Physics Nankai UniversityTianjin 300071 Department o

The prediction of reactor antineutrino spectra will play a crucial role as reactor experiments enter the precision *** positron energy spectrum of 3.5 million antineutrino inverse beta decay reactions observed by the Daya Bay experiment,in combination with the fission rates of fissile isotopes in the reactor,is used to extract the positron energy spectra resulting from the fission of specific *** information can be used to produce a precise,data-based prediction of the antineutrino energy spectrum in other reactor antineutrino experiments with different fission fractions than Daya *** positron energy spectra are unfolded to obtain the antineutrino energy spectra by removing the contribution from detector response with the Wiener-SVD unfolding *** results are obtained with other unfolding methods.A technique to construct a data-based prediction of the reactor antineutrino energy spectrum is proposed and *** the reactor fission fractions,the technique can predict the energy spectrum to a 2%*** addition,we illustrate how to perform a rigorous comparison between the unfolded antineutrino spectrum and a theoretical model prediction that avoids the input model bias of the unfolding method.

关键词： reactor antineutrino energy spectrum Daya Bay application

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High-resolution spectroscopy of the GD-1 stellar stream localizes the perturber near the orbital plane of Sagittarius

arXiv

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arXiv 2020年

作者： Bonaca, Ana Conroy, Charlie Hogg, David W. Cargile, Phillip A. Caldwell, Nelson Naidu, Rohan P. Price-Whelan, Adrian M. Speagle, Joshua S. Johnson, Benjamin D. Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Center for Cosmology and Particle Physics Department of Physics New York University United States Center for Data Science New York University United States Max-Planck-Institut für Astronomie Heidelberg Germany Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue NY10010 United States

The 100◦-long thin stellar stream in the Milky Way halo, GD-1, has an ensemble of features that may be due to dynamical interactions. Using high-resolution MMT/Hectochelle spectroscopy we show that a spur of GD-1-like stars outside of the main stream are kinematically and chemically consistent with the main stream. In the spur, as in the main stream, GD-1 has a low intrinsic radial velocity dispersion, σVr . 1 km s−1, is metal-poor, [Fe/H] ≈ −2.3, with little [Fe/H] spread and some variation in [α/Fe] abundances, which point to a common globular cluster progenitor. At a fixed location along the stream, the median radial velocity offset between the spur and the main stream is smaller than 0.5 km s−1, comparable to the measurement uncertainty. A flyby of a massive, compact object can change orbits of stars in a stellar stream and produce features like the spur observed in GD-1. In this scenario, the radial velocity of the GD-1 spur relative to the stream constrains the orbit of the perturber and its current on-sky position to ≈ 5, 000 deg2. The family of acceptable perturber orbits overlaps the stellar and dark-matter debris of the Sagittarius dwarf galaxy in present-day position and velocity. This suggests that GD-1 may have been perturbed by a globular cluster or an extremely compact dark-matter subhalo formerly associated with Sagittarius. Copyright © 2020, The Authors. All rights reserved.

关键词： Stars

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Observation of spectral lines in the exceptional GRB 221009A

arXiv

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arXiv 2024年

作者： Zhang, Yan-Qiu Xiong, Shao-Lin Mao, Ji-Rong Zhang, Shuang-Nan Xue, Wang-Chen Zheng, Chao Liu, Jia-Cong Zhang, Zhen Wang, Xi-Lu Ge, Ming-Yu Yi, Shu-Xu Song, Li-Ming An, Zheng-Hua Cai, Ce Li, Xin-Qiao Peng, Wen-Xi Tan, Wen-Jun Wang, Chen-Wei Wen, Xiang-Yang Wang, Yue Xiao, Shuo Zhang, Fan Zhang, Peng Zheng, Shi-Jie Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China Yunnan Observatories Chinese Academy of Sciences Yunnan Province Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China College of Physics Hebei Key Laboratory of Photophysics Research and Application Hebei Normal University Hebei Shijiazhuang050024 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China College of Electronic and Information Engineering Tongji University Shanghai201804 China

As the brightest gamma-ray burst ever observed, GRB 221009A provided a precious opportunity to explore spectral line features. In this paper, we performed a comprehensive spectroscopy analysis of GRB 221009A jointly with GECAM-C and Fermi/GBM data to search for emission and absorption lines. For the first time we investigated the line feature throughout this GRB including the most bright part where many instruments suffered problems, and identified prominent emission lines in multiple time intervals. The central energy of the Gaussian emission line evolves from about 37 MeV to 6 MeV, with a nearly constant ratio (about 10%) between the line width and central energy. Particularly, we find that both the central energy and the energy flux of the emission line evolve with time as a power law decay with power law index of -1 and -2 respectively. We suggest that the observed emission lines most likely origin from the blue-shifted electron positron pair annihilation 511 keV line. We find that a standard high latitude emission scenario cannot fully interpret the observation, thus we propose that the emission line comes from some dense clumps with electron positron pairs traveling together with the jet. In this scenario, we can use the emission line to directly, for the first time, measure the bulk Lorentz factor of the jet (Γ) and reveal its time evolution (i.e. Γ ∼ t−1) during the prompt emission. Interestingly, we find that the flux of the annihilation line in the co-moving frame keeps constant. These discoveries of the spectral line features shed new and important lights on the physics of GRB and relativistic jet. Copyright © 2024, The Authors. All rights reserved.

关键词： Gamma rays

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