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arXiv 2021年

作者： Mishra-Sharma, Siddharth Cranmer, Kyle Center for Theoretical Physics Massachusetts Institute of Technology CambridgeMA02139 United States The NSF AI Institute for Artificial Intelligence and Fundamental Interactions Department of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics Harvard University CambridgeMA02138 United States Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY10003 United States Center for Data Science New York University 60 Fifth Ave New YorkNY10011 United States

The nature of the Fermi γ-ray Galactic center Excess (GCE) has remained a persistent mystery for over a decade. Although the excess is broadly compatible with emission expected due to dark matter annihilation, an explanation in terms of a population of unresolved astrophysical point sources e.g., millisecond pulsars, remains viable. The effort to uncover the origin of the GCE is hampered in particular by an incomplete understanding of diffuse emission of Galactic origin. This can lead to spurious features that make it difficult to robustly differentiate smooth emission, as expected for a dark matter origin, from more "clumpy" emission expected from a population of relatively bright, unresolved point sources. We use recent advancements in the field of simulation-based inference, in particular density estimation techniques using normalizing flows, in order to characterize the contribution of modeled components, including unresolved point source populations, to the GCE. Compared to traditional techniques based on the statistical distribution of photon counts, our machine learning-based method is able to utilize more of the information contained in a given model of the Galactic center emission, and in particular can perform posterior parameter estimation while accounting for pixel-to-pixel spatial correlations in the γ-ray map. This makes the method demonstrably more resilient to certain forms of model misspecification. On application to Fermi data, the method generically attributes a smaller fraction of the GCE flux to unresolved point sources when compared to traditional approaches. We nevertheless infer such a contribution to make up a non-negligible fraction of the GCE across all analysis variations considered, with at least 38+9−19% of the excess attributed to unresolved point sources in our baseline analysis. Copyright © 2021, The Authors. All rights reserved.

关键词： Pixels

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Moments for positivity: using Drell-Yan data to test positivity bounds and reverse-engineer new physics

arXiv

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arXiv 2022年

作者： Li, Xu Mimasu, Ken Yamashita, Kimiko Yang, Chengjie Zhang, Cen Zhou, Shuang-Yong Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China School of Physical Sciences University of Chinese Academy of Sciences Beijing100049 China Theoretical Particle Physics and Cosmology Group Department of Physics King's College London LondonWC2R 2LS United Kingdom Department of Physics Chung-Ang University Seoul06974 Korea Republic of Center for High Energy Physics Peking University Beijing100871 China Interdisciplinary Center for Theoretical Study University of Science and Technology of China Anhui Hefei230026 China Peng Huanwu Center for Fundamental Theory Anhui Hefei230026 China

Moments of the leptonic angular distribution in the Drell-Yan process have recently been shown to be sensitive probes of a specific class of dimension-8, four-fermion operators in the Standard Model Effective Field Theory, involving a pair of quarks and leptons. The same operators are also subject to positivity bounds, when requiring the associated (unknown) UV completion to obey basic principles of quantum field theory. We perform a phenomenological study to quantify the sensitivity of the high-luminosity LHC to this set of operators and, by extension, the positivity bounds. We further extend the angular basis of moments and consider double differential information to improve the ability to disentangle the different operators, leading to a sensitivity to new physics scales up to 3 TeV. We use this information to explore the violation of positivity at the LHC as a way to test the underlying principles of quantum field theory. Finally, we present a case study which combines our results with information from other (current and prospective) experiments, as well as the positivity cone to infer the properties of possible tree-level UV completions. The data lead to robust, model-independent lower bounds on the M/√g combination of the particle mass and coupling, for states that couple to right-handed leptons and/or up quarks. Copyright © 2022, The Authors. All rights reserved.

关键词： Angular distribution

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Template bank for compact binary mergers in the fourth observing run of Advanced LIGO, Advanced Virgo, and KAGRA

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Physical Review D 2024年第4期109卷 044066-044066页

作者： Shio Sakon Leo Tsukada Heather Fong James Kennington Wanting Niu Chad Hanna Shomik Adhicary Pratyusava Baral Amanda Baylor Kipp Cannon Sarah Caudill Bryce Cousins Jolien D. E. Creighton Becca Ewing Richard N. George Patrick Godwin Reiko Harada Yun-Jing Huang Rachael Huxford Prathamesh Joshi Soichiro Kuwahara Alvin K. Y. Li Ryan Magee Duncan Meacher Cody Messick Soichiro Morisaki Debnandini Mukherjee Alex Pace Cort Posnansky Anarya Ray Surabhi Sachdev Divya Singh Ron Tapia Takuya Tsutsui Koh Ueno Aaron Viets Leslie Wade Madeline Wade Jonathan Wang Department of Physics The Pennsylvania State University University Park Pennsylvania 16802 USA Institute for Gravitation and the Cosmos The Pennsylvania State University University Park Pennsylvania 16802 USA Department of Physics and Astronomy University of British Columbia Vancouver British Columbia V6T 1Z4 Canada RESCEU The University of Tokyo Tokyo 113-0033 Japan Graduate School of Science The University of Tokyo Tokyo 113-0033 Japan Department of Astronomy and Astrophysics The Pennsylvania State University University Park Pennsylvania 16802 USA Institute for Computational and Data Sciences The Pennsylvania State University University Park Pennsylvania 16802 USA Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA Department of Physics University of Massachusetts Dartmouth Massachusetts 02747 USA Center for Scientific Computing and Data Science Research University of Massachusetts Dartmouth Massachusetts 02747 USA Department of Physics University of Illinois Urbana Illinois 61801 USA Center for Gravitational Physics University of Texas at Austin Austin Texas 78712 USA LIGO Laboratory California Institute of Technology Pasadena California 91125 USA MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology Cambridge Massachusetts 02139 USA Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba 277-8582 Japan NASA Marshall Space Flight Center Huntsville Alabama 35811 USA Center for Space Plasma and Aeronomic Research University of Alabama in Huntsville Huntsville Alabama 35899 USA School of Physics Georgia Institute of Technology Atlanta Georgia 30332 USA Concordia University Wisconsin Mequon Wisconsin 53097 USA Department of Physics Hayes Hall Kenyon College Gambier Ohio 43022 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA

Matched-filtering gravitational-wave search pipelines identify gravitational-wave signals by computing correlations, i.e., signal-to-noise ratios, between gravitational-wave detector data and gravitational-wave template waveforms. Intrinsic parameters, the component masses and spins, of the gravitational-wave waveforms are often stored in “template banks,” and the construction of a densely populated template bank is essential for some gravitational-wave search pipelines. This paper presents a template bank that is currently being used by the GstLAL-based compact binary search pipeline in the fourth observing run of the LIGO, Virgo, and KAGRA collaboration, and was generated with a new binary tree approach of placing templates, manifold. The template bank contains 1.8×106 sets of template parameters covering plausible neutron star and black hole systems up to a total mass of 400M⊙ with component masses between 1–200M⊙ and mass ratios between 1 and 20 under the assumption that each component object’s angular momentum is aligned with the orbital angular momentum. We validate the template bank generated with our new method, manifold, by comparing it with a template bank generated with the previously used stochastic template placement method. We show that both template banks have similar effectualness. The GstLAL search pipeline performs singular value decomposition (SVD) on the template banks to reduce the number of filters used. We describe a new grouping of waveforms that improves the computational efficiency of SVD by nearly 5 times as compared to previously reported SVD sorting schemes.

关键词： General relativity Gravitation Gravitational wave detection Gravitational waves data analysis

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Evidence for PeV Proton Acceleration from Fermi-LAT Observations of SNR G106.3+2.7

arXiv

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arXiv 2022年

作者： Fang, Ke Kerr, Matthew Blandford, Roger Fleischhack, Henrike Charles, Eric Department of Physics Wisconsin IceCube Particle Astrophysics Center University of Wisconsin MadisonWI53706 United States Space Science Division Naval Research Laboratory WashingtonDC20375 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Department of Physics Catholic University of America WashingtonDC20064 United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA GSFC GreenbeltMD20771 United States

The existence of a "knee" at energy ∼ 1 PeV in the cosmic-ray spectrum suggests the presence of Galactic PeV proton accelerators called "PeVatrons". Supernova Remnant (SNR) G106.3+2.7 is a prime candidate for one of these. The recent detection [1-4] of Very High Energy (VHE;0.1-100 TeV) gamma rays from G106.3+2.7 may be explained either by the decay of neutral pions or inverse Compton scattering by relativistic electrons. We report an analysis of 12 years of Fermi-LAT [5] gamma-ray data which shows that the GeV-TeV gamma-ray spectrum is much harder and requires a different total electron energy than the radio and X-ray spectra, suggesting it has a distinct, hadronic origin. The non-detection of gamma rays below 10 GeV implies additional constraints on the relativistic electron spectrum. A hadronic interpretation of the observed gamma rays is strongly supported. This observation confirms the long-sought connection between Galactic PeVatrons and SNRs. Moreover, it suggests that G106.3+2.7 could be the brightest member of a new population of SNRs whose gamma-ray energy flux peaks at TeV energies. Such a population may contribute to the cosmic-ray knee and be revealed by future VHE gamma-ray detectors. © 2022, CC BY.

关键词： Gamma rays

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Gravitational Wave Astronomy With TianQin

arXiv

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arXiv 2024年

作者： Li, En-Kun Liu, Shuai Torres-Orjuela, Alejandro Chen, Xian Inayoshi, Kohei Wang, Long Hu, Yi-Ming Amaro-Seoane, Pau Askar, Abbas Bambi, Cosimo Capelo, Pedro R. Chen, Hong-Yu Chua, Alvin J.K. Condés-Breña, Enrique Dai, Lixin Das, Debtroy Derdzinski, Andrea Fan, Hui-Min Fujii, Michiko Gao, Jie Garg, Mudit Ge, Hongwei Giersz, Mirek Huang, Shun-Jia Hypki, Arkadiusz Liang, Zheng-Cheng Liu, Bin Liu, Dongdong Liu, Miaoxin Liu, Yunqi Mayer, Lucio Napolitano, Nicola R. Peng, Peng Shao, Yong Shashank, Swarnim Shen, Rongfeng Tagawa, Hiromichi Tanikawa, Ataru Toscani, Martina Vázquez-Aceves, Verónica Wang, Hai-Tian Wang, Han Yi, Shu-Xu Zhang, Jian-Dong Zhang, Xue-Ting Zhu, Lianggui Zwick, Lorenz Huang, Song Mei, Jianwei Wang, Yan Xie, Yi Zhang, Jiajun Luo, Jun School of Physics and Astronomy Sun Yat-sen University Zhuhai Campus Zhuhai519082 China MOE Key Laboratory of TianQin Mission TianQin Research Center for Gravitational Physics & Frontiers Science Center for TianQin Gravitational Wave Research Center of CNSA Sun Yat-sen University Zhuhai Campus Zhuhai519082 China School of Electronic and Electrical Engineering Zhaoqing University Zhaoqing526061 China Department of Physics The University of Hong Kong Pokfulam Road Hong Kong The Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Institute for Multidisciplinary Mathematics Polytechnic University of València València46022 Spain Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Warsaw00-716 Poland Center for Astronomy and Astrophysics Center for Field Theory and Particle Physics Department of Physics Fudan University Shanghai200438 China School of Natural Sciences and Humanities New Uzbekistan University Tashkent100007 Uzbekistan Department of Astrophysics University of Zurich Winterthurerstrasse 190 ZürichCH-8057 Switzerland Department of Physics National University of Singapore Singapore117551 Singapore Department of Mathematics National University of Singapore Singapore119076 Singapore Department of Life and Physical Sciences Fisk University Nashville37208 United States Department of Physics & Astronomy Vanderbilt University Nashville37235 United States College of Physics Science & Technology Hebei University Baoding071002 China Department of Astronomy University of Tokyo Tokyo113-0033 Japan Yunnan Observatory Kunming650216 China School of Science Sun Yat-sen University Shenzhen Campus Shenzhen518107 China School of Physics Zhejiang University Hangzhou310027 China Center for Gravitation and Cosmology Yangzhou University Yangzhou225009 China Department of Physics University of Naples Federico II Naples80131 Italy School of Astronomy and Space Science Nanjing210093 China Shang

The opening of the gravitational wave window has significantly enhanced our capacity to explore the universe’s most extreme and dynamic sector. In the mHz frequency range, a diverse range of compact objects, from the most massive black holes at the farthest reaches of the Universe to the lightest white dwarfs in our cosmic backyard, generate a complex and dynamic symphony of gravitational wave signals. Once recorded by gravitational wave detectors, these unique fingerprints have the potential to decipher the birth and growth of cosmic structures over a wide range of scales, from stellar binaries and stellar clusters to galaxies and large-scale structures. The TianQin space-borne gravitational wave mission is scheduled for launch in the 2030s, with an operational lifespan of five years. It will facilitate pivotal insights into the history of our universe. This document presents a concise overview of the detectable sources of TianQin, outlining their characteristics, the challenges they present, and the expected impact of the TianQin observatory on our understanding of them. Copyright © 2024, The Authors. All rights reserved.

关键词： Gravity waves

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First Exploration of Monopole-Driven Shell Evolution above the N=126 Shell Closure: New Millisecond Isomers in Tl213 and Tl215

引用

Physical Review Letters 2024年第7期133卷 072501-072501页

作者： T. T. Yeung A. I. Morales J. Wu M. Liu C. Yuan S. Nishimura V. H. Phong N. Fukuda J. L. Tain T. Davinson K. P. Rykaczewski R. Yokoyama T. Isobe M. Niikura Zs. Podolyák G. Alcalá A. Algora J. M. Allmond J. Agramunt C. Appleton H. Baba R. Caballero-Folch F. Calvino M. P. Carpenter I. Dillmann A. Estrade T. Gao C. J. Griffin R. K. Grzywacz O. Hall Y. Hirayama B. M. Hue E. Ideguchi G. G. Kiss K. Kokubun F. G. Kondev R. Mizuno M. Mukai N. Nepal M. N. Nurhafiza S. Ohta S. E. A. Orrigo M. Pallàs J. Park B. C. Rasco D. Rodríguez-García H. Sakurai L. Sexton Y. Shimizu H. Suzuki A. Vitéz-Sveiczer H. Takeda A. Tarifeno-Saldivia A. Tolosa-Delgado J. A. Victoria Y. X. Watanabe J. M. Yap Department of Physics The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo 113-0033 Japan RIKEN Nishina Center 2-1 Hirosawa Wako Saitama 351-0198 Japan Instituto de Física Corpuscular CSIC-Universitat de València E-46071 València Spain National Nuclear Data Center Brookhaven National Laboratory Upton New York 11973 USA Facility for Rare Isotope Beams Michigan State University East Lansing Michigan 48824 USA Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai Guangdong 519082 China Faculty of Physics University of Science Vietnam National University Hanoi 120062 Vietnam School of Physics and Astronomy University of Edinburgh EH9 3FD Edinburgh United Kingdom Physics Division Oak Ridge National Laboratory Oak Ridge Tennessee 37831-6368 USA Department of Physics and Astronomy University of Tennessee Knoxville Tennessee 37996 USA Center for Nuclear Study the University of Tokyo 2-1 Hirosawa Wako Saitama 351-0198 Japan Department of Physics University of Surrey Guildford Surrey GU2 7XH United Kingdom HUN-REN Institute for Nuclear Research Bem tér 18/c Debrecen H4032 Hungary TRIUMF Vancouver British Columbia V6T 2A3 Canada Universitat Politecnica de Catalunya E-08028 Barcelona Spain Physics Division Argonne National Laboratory Argonne Illinois 60439 USA Department of Physics and Astronomy University of Victoria Victoria British Columbia V8P 5C2 Canada Department of Physics Central Michigan University Mount Pleasant Michigan 48859 USA Department of Physics The University of Hong Kong Pokfulam Hong Kong China Wako Nuclear Science Center (WNSC) Institute of Particle and Nuclear Studies (IPNS) High Energy Accelerator Research Organization (KEK) Wako Saitama 351-0198 Japan Institute of Physics Vietnam Academy of Science and Technology Hanoi 10000 Vietnam Research Center for Nuclear Physics (RCNP) Osaka University 10-1 Mihogaoka Ibaraki Osaka 567-0047 Japan Department of Applied Energy Nagoya University Nag

Isomer spectroscopy of heavy neutron-rich nuclei beyond the N=126 closed shell has been performed for the first time at the Radioactive Isotope Beam Factory of the RIKEN Nishina center. New millisecond isomers have been identified at low excitation energies, 985.3(19) keV in Tl213 and 874(5) keV in Tl215. The measured half-lives of 1.34(5) ms in Tl213 and 3.0(3) ms in Tl215 suggest spins and parities 11/2− with the single proton-hole configuration πh11/2 as leading component. They are populated via E1 transitions by the decay of higher-lying isomeric states with proposed spin and parity 17/2+, interpreted as arising from a single πs1/2 proton hole coupled to the 8+ seniority isomer in the PbA+1 cores. The lowering of the 11/2− states is ascribed to an increase of the πh11/2 proton effective single-particle energy as the second νg9/2 orbital is filled by neutrons, owing to a significant reduction of the proton-neutron monopole interaction between the πh11/2 and νg9/2 orbitals. The new ms isomers provide the first experimental observation of shell evolution in the almost unexplored N>126 nuclear region below doubly magic Pb208.

关键词： Electromagnetic transitions Energy levels Isomer decays Lifetimes & widths Nuclear fragmentation Nuclear structure & decays Shell model 190 ≤ A ≤ 219 Radioactive beams Spectrometers & spectroscopic techniques

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Prospects for exotic h → 4τ decays in single and di-Higgs boson production at the LHC and future hadron colliders

arXiv

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arXiv 2022年

作者： Adhikary, Amit Banerjee, Shankha Barman, Rahool Kumar Batell, Brian Bhattacherjee, Biplob Bose, Camellia Qian, Zhuoni Spannowsky, Michael Institute of Theoretical Physics Faculty of Physics University of Warsaw Pasteura 5 WarsawPL 02-093 Poland Centre for High Energy Physics Indian Institute of Science Bangalore560012 India CERN Theoretical Physics Department Geneva 23CH-1211 Switzerland Department of Physics Oklahoma State University StillwaterOK74078 United States Pittsburgh Particle Physics Astrophysics and Cosmology Center Department of Physics and Astronomy University of Pittsburgh Pittsburgh United States Hangzhou Normal University Zhejiang Hangzhou311121 China Institute for Particle Physics Phenomenology Durham University South Road DurhamDH1 3LE United Kingdom

We study the prospects for observing exotic decays of the Standard Model Higgs boson h into light beyond the Standard Model scalars a with mass ma mh/2 in the single Higgs and Higgs pair production channels at the high luminosity run of the Large Hadron Collider (HL-LHC). Discovery prospects for single Higgs production in the gluon-gluon fusion and vector boson fusion modes with the Higgs boson decaying via the exotic mode h → aa → 4τ are analyzed at the HL-LHC. The projected sensitivity for exotic Higgs decays in the nonresonant Higgs pair production channel pp → hh → (h → bb¯)(h → aa → 4τ) → 2b4τ at the HL-LHC and a future √s = 100 TeV hadron collider (FCC-hh) are also estimated. Furthermore, we study HL-LHC’s potential reach for the Higgs-strahlung process in the 2b4τ channel, taking into account the contamination from nonresonant Higgs pair production. Finally, the potential reach for resonant Higgs pair production in the 2b4τ channel at the HL-LHC is also explored for several choices of {mH, ma}. Our studies suggest that significant improvements over existing bounds are achievable in several production channels, motivating new dedicated searches for h → aa → 4τ at the HL-LHC and future colliders. © 2022, CC BY.

关键词： Bosons

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Modeling phonon-mediated quasiparticle poisoning in superconducting qubit arrays

arXiv

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arXiv 2024年

作者： Yelton, Eric Larson, Clayton P. Iaia, Vito Dodge, Kenneth La Magna, Guglielmo Baity, Paul G. Pechenezhskiy, Ivan V. McDermott, Robert Kurinsky, Noah A. Catelani, Gianluigi Plourde, Britton L.T. Department of Physics Syracuse University SyracuseNY13244-1130 United States Intelligence Community Postdoctoral Research Fellowship Program Department of Physics Syracuse University SyracuseNY13244-1130 United States Forschungszentrum Jülich Jülich52425 Germany Quantum Research Center Technology Innovation Institute Abu Dhabi9639 United Arab Emirates Computational Science Initiative Brookhaven National Laboratory UptonNY11973 United States Department of Physics University of Wisconsin-Madison MadisonWI53706 United States Kavli Institute for Particle Astrophysics and Cosmology SLAC National Accelerator Laboratory Menlo ParkCA94025 United States

Correlated errors caused by ionizing radiation impacting superconducting qubit chips are problematic for quantum error correction. Such impacts generate quasiparticle (QP) excitations in the qubit electrodes, which temporarily reduce qubit coherence significantly. The many energetic phonons produced by a particle impact travel efficiently throughout the device substrate and generate quasiparticles with high probability, thus causing errors on a large fraction of the qubits in an array simultaneously. We describe a comprehensive strategy for the numerical simulation of the phonon and quasiparticle dynamics in the aftermath of an impact. We compare the simulations with experimental measurements of phonon-mediated QP poisoning and demonstrate that our modeling captures the spatial and temporal footprint of the QP poisoning for various configurations of phonon downconversion structures. We thus present a path forward for the operation of superconducting quantum processors in the presence of ionizing radiation. Copyright © 2024, The Authors. All rights reserved.

关键词： Qubits

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Evidence for particle acceleration approaching PeV energies in the W51 complex

arXiv

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arXiv 2024年

作者： Cao, Zhen Aharonian, F. Axikegu Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Bian, W. Bukevich, A.V. Cao, Q. Cao, W.Y. Cao, Zhe Chang, J. Chang, J.F. Chen, A.M. Chen, E.S. Chen, H.X. Chen, Liang Chen, Lin Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, Y. Cheng, N. Cheng, Y.D. Cui, M.Y. Cui, S.W. Cui, X.H. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu Dong, X.Q. Duan, K.K. Fan, J.H. Fan, Y.Z. Fang, J. Fang, J.H. Fang, K. Feng, C.F. Feng, H. Feng, L. Feng, S.H. Feng, X.T. Feng, Y. Feng, Y.L. Gabici, S. Gao, B. Gao, C.D. Gao, Q. Gao, W. Gao, W.K. Ge, M.M. Geng, L.S. Giacinti, G. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. Hasan, M. He, H.H. He, H.N. He, J.Y. He, Y. Hou, B.W. Hou, C. Hou, X. Hu, H.B. Hu, Q. Hu, S.C. Huang, D.H. Huang, T.Q. Huang, W.J. Huang, X.T. Huang, X.Y. Huang, Y. Ji, X.L. Jia, H.Y. Jia, K. Jiang, K. Jiang, X.W. Jiang, Z.J. Jin, M. Kang, M.M. Karpikov, I. Kuleshov, D. Kurinov, K. Li, B.B. Li, C.M. Li, Cheng Li, Cong Li, D. Li, F. Li, H.B. Li, H.C. Li, Jian Li, Jie Li, K. Li, S.D. Li, W.L. Li, W.L. Li, X.R. Li, Xin Li, Y.Z. Li, Zhe Li, Zhuo Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, D. Liu, D.B. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Luo, Q. Luo, Y. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Min, Z. Mitthumsiri, W. Mu, H.J. Nan, Y.C. Neronov, A. Ou, L.J. Pattarakijwanich, P. Pei, Z.Y. Qi, J.C. Qi, M.Y. Qiao, B.Q. Qin, J.J. Raza, A. Ruffolo, D. Sáiz, A. Saeed, M. Semikoz, D. Shao, L. Shchegolev, O. Sheng, X.D. Shu, F.W. Song, H.C. Stenkin, Yu V. Stepanov, V. Su, Y. Sun, D.X. Sun, Q.N. Sun, X.N. Sun, Z.B. Takata, J. Tam, P.H.T. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Chengdu China Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Max-Planck-Institut for Nuclear Physics 69029 Heidelberg103980 Germany School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Chengdu610031 China School of Astronomy and Space Science Nanjing University Nanjing210023 China Center for Astrophysics Guangzhou University Guangzhou510006 China Tsung-Dao Lee Institute School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Institute for Nuclear Research of Russian Academy of Sciences Moscow117312 Russia Hebei Normal University Shijiazhuang050024 China University of Science and Technology of China Hefei230026 China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China Research Center for Astronomical Computing Zhejiang Laboratory Hangzhou311121 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China School of Physics and Astronomy Yunnan University Kunming650091 China Ministry of Education Lhasa850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Sun Yat-sen University Zhuhai 519000 Guangdong Guangzhou510275 China Institute of Frontier and Interdisciplinary Science Shandong University Qingdao266237 China APC Université Paris Cité CNRS IN2P3 CEA/IRFU Observatoire de Paris Paris119 75205 France Department of Engineering Physics Tsinghua Universit

The γ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays (CRs) accelerated by the shock of supernova remnant (SNR) W51C and the dense molecular clouds in the adjacent star-forming region, W51B. However, the maximum acceleration capability of W51C for CRs remains elusive. Based on observations conducted with the Large High Altitude Air Shower Observatory (LHAASO), we report a significant detection of γ rays emanating from the W51 complex, with energies from 2 TeV to 200 TeV. The LHAASO measurements, for the first time, extend the γ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of TeV. By combining the "π0-decay bump" featured data from Fermi-LAT, the broadband γ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision model. The observed spectral bending feature suggests an exponential cutoff at ∼ 400 TeV or a power-law break at ∼ 200 TeV in the CR proton spectrum, most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV regime. Additionally, two young star clusters within W51B could also be theoretically viable to produce the most energetic γ rays observed by LHAASO. Our findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs. © 2024, CC BY.

关键词： Cosmic rays

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IceCube search for neutrinos from GRB 221009A

IceCube search for neutrinos from GRB 221009A

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Anton, G. Argüelles, C. Ashida, Y. Athanasiadou, S. Axani, S.N. Bai, X. Balagopal, A.V. Baricevic, M. Barwick, S.W. Basu, V. Bay, R. Beatty, J.J. Becker Tjus, J. Beise, J. Bellenghi, C. Benning, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Blaufuss, E. Blot, S. Bontempo, F. Book, J.Y. Boscolo Meneguolo, C. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Braun, J. Brinson, B. Brostean-Kaiser, J. Burley, R.T. Busse, R.S. Butterfield, D. Campana, M.A. Carloni, K. Carnie-Bronca, E.G. Chattopadhyay, S. Chau, N. Chen, C. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Classen, L. Coleman, A. Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Dave, P. De Clercq, C. DeLaunay, J.J. Delgado, D. Deng, S. Deoskar, K. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Domi, A. Dujmovic, H. DuVernois, M.A. Ehrhardt, T. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. 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. Fritz, A. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goehlke, N. Gonzalez, J.G. Goswami, S. Grant, D. Gray, S.J. Gries, O. Griffin, S. Griswold, S. Groth, K.M. Günther, C. Gutjahr, P. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Hamdaoui, H. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haungs, A. Helbing, K. Hellrung, J. Henningsen, F. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hill, C. Hill, G.C. Hoffman, K.D. Hori, S. Hoshina, K. Hou, W. Huber, T. Hultqvist, K. Hünnefeld, M. Hussain, R. Hymon, K. In, S. Ishihara, A. Jacquart, M. Janik, O. Jansson, M. Japaridze, G.S. Jeong, 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 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 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 Astro

GRB 221009A is the brightest Gamma Ray Burst (GRB) ever observed. The observed extremely high flux of high and very-high-energy photons provide a unique opportunity to probe the predicted neutrino counterpart to the electromagnetic emission. We have used a variety of methods to search for neutrinos in coincidence with the GRB over several time windows during the precursor, prompt and afterglow phases of the GRB. MeV scale neutrinos are studied using photo-multiplier rate scalers which are normally used to search for galactic core-collapse supernovae neutrinos. GeV neutrinos are searched starting with DeepCore triggers. These events don’t have directional localization, but instead can indicate an excess in the rate of events. 10 GeV - 1 TeV and >TeV neutrinos are searched using traditional neutrino point source methods which take into account the direction and time of events with DeepCore and the entire IceCube detector respectively. The >TeV results include both a fast-response analysis conducted by IceCube in real-time with time windows of T0 - 1 to T0 + 2 hours and T0 ± 1 day around the time of GRB 221009A, as well as an offline analysis with 3 new time windows up to a time window of T0 - 1 to T0 + 14 days, the longest time period we consider. The combination of observations by IceCube covers 9 orders of magnitude in neutrino energy, from MeV to PeV, placing upper limits across the range for predicted neutrino emission. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Supernovae

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