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Design and performance of the multi-PMT optical module for IceCube Upgrade 37

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Design and performance of the multi-PMT optical module for I...

37th International Cosmic Ray Conference, ICRC 2021

作者： Anderson, T. Classen, L. Fienberg, A.T. Mechbal, S. Schneider, J. Sulanke, K.-H. Unland Elorrieta, M.A. Wendt, C. 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. Dept. of Physics Pennsylvania State University University Park United States Institut für Kernphysik Westfälische Wilhelms-Universität Münster Münster Germany DESY Zeuthen Germany Erlangen Centre for Astroparticle Physics Erlangen Germany Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center University of Wisconsin–Madison 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

The IceCube Upgrade is the first step towards the next-generation neutrino observatory at the South Pole, IceCube-Gen2, and will be installed in the central region of the existing array. The Upgrade will consist of 693 newly developed, densely spaced optical sensors and 50 standalone calibration devices, which will enhance IceCube’s capabilities both at low and high neutrino energies. Of the new sensors, 402 will be multi-PMT Digital Optical Modules (mDOMs). Consisting of 24 small photomultipliers arranged inside a pressure vessel, the mDOM features a large sensitive area distributed nearly homogeneously over the full solid angle. The use of multiple, individually read-out PMTs allows directional information to be obtained for the registered photons and enables the use of multiplicity triggering within a single module, e.g., for background suppression. The challenges driving the mDOM development included tight restrictions on module size, data-transfer rate, and power consumption as well as the harsh environment in the deep ice at the South Pole. In this contribution we present the final mDOM design that meets these challenges. © Copyright owned by the author(s).

关键词： data transfer

SOFIA/HAWC+ FAR-INFRARED POLARIMETRIC LARGE-AREA CMZ EXPLORATION SURVEY. IV. RELATIVE MAGNETIC FIELD ORIENTATION THROUGHOUT THE CMZ

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arXiv 2024年

作者： Paré, Dylan M. Chuss, David T. Karpovich, Kaitlyn Butterfield, Natalie O. Iuliano, Jeffrey Inara Pan, Xing Wollack, Edward J. Zhang, Qizhou Morris, Mark R. Nilsson, Mathilda Zhao, Roy J. Department of Physics Villanova University 800 E. Lancaster Ave. VillanovaPA19085 United States Department of Physics Stanford University StanfordCA94305 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P.O. Box 2450 StanfordCA94305 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States School of Astronomy and Space Science Nanjing University 163 Xianlin Avenue Nanjing210023 China Ministry of Education Nanjing210023 China Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States NASA Goddard Space Flight Center Mail Code: 665 GreenbeltMD20771 United States Department of Physics & Astronomy University of California Los Angeles 475 Portola Pl. Los AngelesCA90095-1547 United States Department of Physics and Astronomy University of Pittsburgh 100 Allen Hall 3941 O’Hara St. PittsburghPA15260 United States Kavli Institute for Cosmological Physics The University of Chicago 5640 S Ellis Ave. ChicagoIL60637 United States Department of Physics The University of Chicago 5720 S Ellis Ave. ChicagoIL60637 United States

The nature of the magnetic field structure throughout the Galactic center (GC) has long been of interest. The recent Far-InfraREd Polarimetric Large-Area CMZ Exploration (FIREPLACE) Survey reveals preliminary connections between the seemingly distinct vertical and horizontal magnetic field distributions previously observed in the GC. We use the statistical techniques of the Histogram of Relative Orientation (HRO) and the Projected Rayleigh Statistic (PRS) to assess whether the CMZ magnetic field preferentially aligns with the structure of the CMZ molecular clouds or the morphology of the non-thermal emission of the GC NTF population. We find that there is a range of magnetic field orientations throughout the population of CMZ molecular clouds, ranging from parallel to perpendicular orientation. We posit these orientations depend on the prevalence of gravitational shear in the GC in contrast with what is observed in Galactic Disk star-forming regions. We also compare the magnetic field orientation from dust polarimetry with individual prominent NTFs, finding a preferred perpendicular relative orientation. This perpendicular orientation indicates that the vertical field component found in the FIREPLACE observations is not spatially confined to the NTFs, providing evidence for a more pervasive vertical field in the GC. From dynamical arguments, we estimate an upper limit on the magnetic field strength for this vertical field, finding B ≤ 4 mG. A field close to this upper limit would indicate that the NTFs are not local enhancements of a weaker background field and that the locations of the NTFs depend on proximity to sites of cosmic ray production. © 2024, CC BY.

关键词： cosmology

Measurement of atmospheric neutrino mixing with improved IceCube DeepCore calibration and data processing

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Physical Review D 2023年第1期108卷 012014-012014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 V. M. Baricevic S. W. Barwick V. Basu R. Bay J. J. Beatty K.-H. Becker J. Becker Tjus J. Beise C. Bellenghi C. Benning S. BenZvi D. Berley E. Bernardini D. Z. Besson G. Binder 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 H. Dembinski S. Deng 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 P. Eller S. El Mentawi R. Engel H. Erpenbeck J. Evans P. A. Evenson K. L. Fan K. Fang K. Farrag 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 O. Gries S. Griffin 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 N. Heyer S. Hickford A. Hidvegi J. Hignight C. Hill G. C. Hill K. D. Hoffman S. Hori K. Hoshina W. Hou T. Huber K. Hultqvist M. Hünnefeld R. Hussain K. Hymon S. In A. Ishihara M. Jacquart O. Janik 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. Khatee Zathul A. Kheirandish J. Kiryluk S. R. Klein A. Kochocki 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 & 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 III. Physikalisches Institut RWTH Aachen University D-52056 Aachen Germany Department of Physics and Astronomy University of Rochester Rochester New York 14627 USA Depa

We describe a new data sample of IceCube DeepCore and report on the latest measurement of atmospheric neutrino oscillations obtained with data recorded between 2011–2019. The sample includes significant improvements in data calibration, detector simulation, and data processing, and the analysis benefits from a sophisticated treatment of systematic uncertainties, with significantly greater level of detail since our last study. By measuring the relative fluxes of neutrino flavors as a function of their reconstructed energies and arrival directions we constrain the atmospheric neutrino mixing parameters to be sin2θ23=0.51±0.05 and Δm322=2.41±0.07×10−3 eV2, assuming a normal mass ordering. The errors include both statistical and systematic uncertainties. The resulting 40% reduction in the error of both parameters with respect to our previous result makes this the most precise measurement of oscillation parameters using atmospheric neutrinos. Our results are also compatible and complementary to those obtained using neutrino beams from accelerators, which are obtained at lower neutrino energies and are subject to different sources of uncertainties.

关键词： Neutrino oscillations

One small step for an inflaton, one giant leap for inflation: a novel non-Gaussian tail and primordial black holes

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arXiv 2021年

作者： Cai, Yi-Fu Ma, Xiao-Han Sasaki, Misao Wang, Dong-Gang Zhou, Zihan Department of Astronomy School of Physical Sciences University of Science and Technology of China Anhui Hefei230026 China CAS Key Laboratory for Researches in Galaxies and Cosmology School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China UTIAS The University of Tokyo Chiba277-8583 Japan Center for Gravitational Physics Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road CambridgeCB3 0WA United Kingdom Department of Physics Princeton University PrincetonNJ08544 United States

We report a novel prediction from single-field inflation that even a tiny step in the inflaton potential can change our perception of primordial non-Gaussianities of the curvature perturbation. Our analysis focuses on the tail of probability distribution generated by an upward step transition between two stages of slow-roll evolution. The nontrivial background dynamics with off-attractor behavior is identified. By using a non-perturbative δN analysis, we explicitly show that a highly non-Gaussian tail can be generated by a tiny upward step, even when the conventional nonlinearity parameters fNLlocal, gNLlocal, etc. remain small. With this example, we demonstrate for the first time the sensitive dependence of non-perturbative effects on the tail of probability distribution. Our scenario has an inconceivable application to primordial black holes by either significantly boosting their abundance or completely forbidding their appearance. © 2021, CC BY.

关键词： Gravitation

Transition edge sensor based detector: from X-ray to γ-ray

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arXiv 2022年

作者： Zhang, Shuo Xia, Jing-Kai Sun, Tao Wu, Wen-Tao Wu, Bing-Jun Wang, Yong-Liang Cantor, Robin Han, Ke Zhou, Xiao-Peng Liu, Hao-Ran Fan, Fu-You Guo, Si-Ming Liang, Jun-Cheng Li, De-Hong Song, Yan-Ru Ju, Xu-Dong Fu, Qiang Liu, Zhi Center for Transformative Science ShanghaiTech University ShangHai 201210 China Shanghai Institute of Microsystem and Information Technology Chinese Academy of Sciences ShangHai 200050 China STAR Cryoelectronics 25-A Bisbee Court Santa FeNM87508-1338 United States INPAC Department of Physics and Astronomy Shanghai Jiao Tong University Shanghai Laboratory for Particle Physics and Cosmology Shanghai 200240 China School of Physics Beihang University Beijing100191 China Division of Ionizing Radiation National Institute of Metrology NIM No.18 Bei San Huan Dong Lu Chaoyang Dist Beijing100029 China

The Transition Edge Sensor is extremely sensitive to the change of temperature, combined with the high-Z metal of a certain thickness, it can realize the high energy resolution measurement of particles such as X-rays. X-rays with energies below 10 keV have very weak penetrating ability, so only a few microns thick of gold or bismuth can obtain quantum efficiency higher than 70%. Therefore, the entire structure of the TES X-ray detector in this energy range can be realized in the microfabrication process. However, for X-rays or gamma rays from 10 keV to 200 keV, sub-millimeter absorber layers are required, which cannot be realized by microfabrication process. This paper first briefly introduces a set of TES X-ray detectors and their auxiliary systems built by ShanghaiTech University, then focus on the introduction of the TES γ-ray detector, with absorber based on an sub-millimeter lead-tin alloy sphere. The detector has a quantum efficiency above 70% near 100 keV, and an energy resolution of about 161.5eV@*** Codes 81V35 Copyright © 2022, The Authors. All rights reserved.

关键词： X ray detectors

Latest Results from the Daya Bay Experiment 37

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Latest Results from the Daya Bay Experiment

37th International Cosmic Ray Conference, ICRC 2021

作者： Dohnal, Tadeáš An, F.P. Balantekin, A.B. Bishai, M. Blyth, S. Cao, G.F. Cao, J. Chang, J.F. Chang, Y. Chen, H.S. Chen, S.M. Chen, Y. Chen, Y.X. Cheng, J. Cheng, Z.K. Cherwinka, J.J. Chu, M.C. Cummings, J.P. Dalager, O. Deng, F.S. Ding, Y.Y. Diwan, M.V. Dohal, T. Dolzhikov, D. Dove, J. Dvořák, M. Dwyer, D.A. Gallo, J.P. Gonchar, M. Gong, G.H. Gong, H. Grassi, M. Gu, W.Q. Guo, J.Y. Guo, L. Guo, X.H. Guo, Y.H. Guo, Z. Hackenburg, R.W. Hans, S. He, M. Heeger, K.M. Heng, Y.K. Higuera, A. Hor, Y.K. Hsiung, Y.B. Hu, B.Z. Hu, J.R. Hu, T. Hu, Z.J. Huang, H.X. Huang, J.H. Huang, X.T. Huang, Y.B. Huber, P. Jaffe, D.E. Jen, K.L. Ji, X.L. Ji, X.P. Johnson, R.A. Jones, D. Kang, L. Kettell, S.H. Kohn, S. Kramer, M. Langford, T.J. Lee, J. Lee, J.H.C. Lei, R.T. Leitner, R. Leung, J.K.C. Li, 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. Liang, H. Lin, C.J. Lin, G.L. Lin, S. Ling, J.J. Link, J.M. Littenberg, L. Littlejohn, B.R. Liu, J.C. Liu, J.L. Liu, J.X. Lu, C. Lu, H.Q. Lu, J.S. Luk, K.B. Ma, B.Z. Ma, X.B. Ma, X.Y. Ma, Y.Q. Mandujano, R.C. Marshall, C. McDonald, K.T. McKeown, R.D. Meng, Y. Napolitano, J. Naumov, D. Naumova, E. Nguyen, T.M.T. Ochoa-Ricoux, J.P. Olshevskiy, A. Pan, H.-R. Park, J. Patton, S. Peng, J.C. Pun, C.S.J. Qi, F.Z. Qi, M. Qian, X. Raper, N. Ren, J. Morales Reveco, C. Rosero, R. Roskovec, B. Ruan, X.C. Steiner, H. Sun, J.L. Tmej, T. Treskov, K. Tse, W.-H. Tull, C.E. Viren, B. Vorobel, V. Wang, 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. Wei, H.Y. Wei, L.H. Wen, L.J. Whisnant, K. White, C.G. Wong, H.L.H. Worcester, E. Wu, D.R. Wu, F.L. Wu, Q. Wu, W.J. Xia, D.M. Xie, Z.Q. Xing, Z.Z. Xu, H.K. Xu, J.L. Xu, T. Xue, T. Yang, C.G. Yang, L. Yang, Y.Z. Yao, H.F. Ye, M. Institute of Particle and Nuclear Physics Faculty of Mathematics and Physics Charles University V Holešovičkách 2 Prague 8180 00 Czech Republic Institute of Modern Physics East China University of Science and Technology Shanghai China University of Wisconsin MadisonWI53706 United States Brookhaven National Laboratory UptonNY11973 United States Department of Physics National Taiwan University Taipei Taiwan Institute of High Energy Physics Beijing China National United University Miao-Li Liechtenstein Department of Engineering Physics Tsinghua University Beijing China Shenzhen University Shenzhen China University Guangzhou China North China Electric Power University Beijing China Chinese University of Hong Kong Hong Kong Siena College LoudonvilleNY12211 United States Department of Physics and Astronomy University of California IrvineCA92697 United States University of Science and Technology of China Hefei China Charles University Faculty of Mathematics and Physics Prague Czech Republic Joint Institute for Nuclear Research Moscow Region Dubna Russia Department of Physics University of Illinois at Urbana-Champaign UrbanaIL61801 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics Illinois Institute of Technology ChicagoIL60616 United States Beijing Normal University Beijing China Department of Nuclear Science and Technology School of Energy and Power Engineering Xi’an Jiaotong University Xi’an China Wright Laboratory Department of Physics Yale University New HavenCT06520 United States Department of Physics University of Houston HoustonTX77204 United States China Institute of Atomic Energy Beijing China Shandong University Jinan China Guangxi University No.100 Daxue East Road Nanning China Center for Neutrino Physics Virginia Tech BlacksburgVA24061 United States Institute of Physics National Chiao-Tung University Hsinchu Taiwan Department of Physics University of Cincinna

The Daya Bay Reactor Neutrino Experiment, located in southeast China, was designed to measure short baseline oscillation of electron antineutrinos originating from six 2.9 GWth nuclear reactors. Since 2011, it has collected an unprecedented sample of millions of reactor antineutrino candidates, the largest sample in the world up to date, which led to the discovery of the non-zero θ13 mixing angle just in 2012. In this talk, we present an overview of the latest results from Daya Bay including the measurement of oscillation parameters driving the reactor antineutrino disappearance at short baseline, with the most precise measurement of the θ13 mixing angle in the world, search for light sterile neutrino mixing, and search for electron antineutrinos associated with gravitational wave events among others. © Copyright owned by the author(s).

关键词： Gravity waves

COOL-LAMPS. VII. Quantifying Strong-lens Scaling Relations with 177 Cluster-scale Strong Gravitational Lenses in DECaLS

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arXiv 2024年

作者： Mork, Simon D. Gladders, Michael D. Khullar, Gourav Sharon, Keren Chicoine, Nathalie Cloonan, Aidan P. Dahle, Håkon Garza, Diego Glusman, Rowen Gozman, Katya Horwath, Gabriela Levine, Benjamin C. Liang, Olina Mahronic, Daniel Manwadkar, Viraj Martinez, Michael N. Masegian, Alexandra Matthews Acuña, Owen S. Merz, Kaiya Pan, Yue Sanchez, Jorge A. Sierra, Isaac Kavin Stein, Daniel J. Sukay, Ezra Tamargo-Arizmendi, Marcos Tavangar, Kiyan Tu, Ruoyang Wagner, Grace Zaborowski, Erik A. Zhang, Yunchong Department of Astronomy and Astrophysics University of Chicago 5640 S. Ellis Avenue ChicagoIL60637 United States School of Earth and Space Exploration Arizona State University 781 Terrace Mall TempeAZ85287 United States Beus Center for Cosmic Foundations Arizona State University 781 Terrace Mall TempeAZ85287 United States Kavli Institute for Cosmological Physics University of Chicago 5640 S. Ellis Avenue ChicagoIL60637 United States Department of Physics and Astronomy University of Pittsburgh 3941 O’Hara Street PittsburghPA15260 United States Pittsburgh Particle Physics Astrophysics and Cosmology Center University of Pittsburgh 3941 O’Hara Street PittsburghPA15260 United States Department of Astronomy University of Michigan 1085 S. University Avenue Ann ArborMI48109 United States Department of Astronomy University of Massachusetts Amherst 710 N. Pleasant Street AmherstMA01003 United States Institute of Theoretical Astrophysics University of Oslo P.O. Box 1029 Blindern OsloNO-0315 Norway Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Gravitation & Astroparticle Physics University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Department of Physics and Astronomy Stony Brook University 100 Nicolls Road Stony BrookNY11794 United States Department of Physics Stanford University 382 Via Pueblo StanfordCA94305 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University 382 Via Pueblo StanfordCA94305 United States Department of Physics University of Wisconsin Madison 1150 University Avenue MadisonWI53706 United States Department of Astronomy Columbia University 538 W. 120th Street New YorkNY10027 United States Department of Astronomy University of Wisconsin—Madison 475 N. Charter Street MadisonWI53706 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department

We estimate the Einstein-radius-enclosed total mass for 177 cluster-scale strong gravitational lenses identified by the ChicagO Optically selected Lenses Located At the Margins of Public Surveys (COOL-LAMPS) collaboration with lens redshifts ranging from 0.2 z 1.0 using the brightest-cluster-galaxy (BCG) redshift and an observable proxy for the Einstein radius. We constrain the Einstein-radius-enclosed luminosity and stellar mass by fitting parametric spectral energy distributions to aperture photometry from the Dark Energy Camera Legacy Survey in the g-, r-, and z-band Dark Energy Camera filters. We find that the BCG redshift, enclosed total mass, and enclosed luminosity are strongly correlated and well described by a planar relationship in 3D space. We find that the enclosed total mass and stellar mass are correlated with a logarithmic slope of 0.500+0−0.029031, and the enclosed total mass and stellar-to-total mass fraction are correlated with a logarithmic slope of −0.495+0−0.032033. In tandem with the small radii within which these slopes are constrained, this may suggest invariance in baryon conversion efficiency and feedback strength as a function of cluster-centric radii in galaxy clusters. Additionally, the correlations described here should have utility in ranking strong-lensing candidates in upcoming imaging surveys—such as Rubin/Legacy Survey of Space and Time—in which an algorithmic treatment of strong lenses will be needed due to the sheer volume of data these surveys will produce. © 2024, CC BY.

关键词： Dark energy

Measurement of the inelasticity distribution of neutrino-nucleon interactions for 80 GeV ν < 560 GeV with IceCube DeepCore

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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

GRTresna: An open-source code to solve the initial data constraints in numerical relativity

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arXiv 2025年

作者： Aurrekoetxea, Josu C. Brady, Sam E. Aresté-Saló, Llibert Bamber, Jamie Chung-Jukko, Liina Clough, Katy de Jong, Eloy Elley, Matthew Figueras, Pau Helfer, Thomas Lim, Eugene A. Radia, Miren Waeming, Areef Wang, Zipeng Center for Theoretical Physics Massachusetts Institute of Technology 77 Massachusetts Ave CambridgeMA02139 United States School of Mathematical Sciences Queen Mary University of London Mile End Road LondonE1 4NS United Kingdom Institute for Theoretical Physics KU Leuven Celestijnenlaan 200D LeuvenB-3001 Belgium Leuven Gravity Institute KU Leuven Celestijnenlaan 200D LeuvenB-3001 Belgium Department of Physics University of Illinois Urbana-Champaign UrbanaIL61801 United States Theoretical Particle Physics and Cosmology Group Physics Department King’s College London Strand LondonWC2R 2LS United Kingdom Department of Physics University of Basque Country UPV/EHU Bilbao48080 Spain Institute for Advanced Computational Science Stony Brook University NY11794 United States Information Services University of Cambridge Roger Needham Building 7 JJ Thomson Avenue CambridgeCB3 0WA United Kingdom Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States

GRTresna is a multigrid solver designed to solve the constraint equations for the initial data required in numerical relativity simulations. In particular it is focussed on scenarios with fundamental fields around black holes and inhomogeneous cosmological spacetimes. The following overview has been prepared as part of the submission of the code to the Journal of Open Source Software. The code is based on the formalism in Aurrekoetxea, Clough & Lim [1] and can be found at https://***/GRTLCollaboration/GRTresna1 © 2025, CC BY.

关键词： Relativity