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Microlensing events indicate that super-Earth exoplanets are common in Jupiter-like orbits

science (New York, N.Y.) 2025年第6745期388卷 400-404页

作者： Zang, Weicheng Jung, Youn Kil Yee, Jennifer C. Hwang, Kyu-Ha Yang, Hongjing Udalski, Andrzej Sumi, Takahiro Gould, Andrew Mao, Shude Albrow, Michael D. Chung, Sun-Ju Han, Cheongho Ryu, Yoon-Hyun Shin, In-Gu Shvartzvald, Yossi Cha, Sang-Mok Kim, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Lee, Chung-Uk Lee, Dong-Joo Lee, Yongseok Park, Byeong-Gon Pogge, Richard W. Zhang, Xiangyu Kuang, Renkun Wang, Hanyue Zhang, Jiyuan Hu, Zhecheng Zhu, Wei Mróz, Przemek Skowron, Jan Poleski, Radosław Szymański, Michał K Soszyński, Igor Pietrukowicz, Paweł Kozłowski, Szymon Ulaczyk, Krzysztof Rybicki, Krzysztof A. Iwanek, Patryk Wrona, Marcin Gromadzki, Mariusz Abe, Fumio Barry, Richard Bennett, David P. Bhattacharya, Aparna Bond, Ian A. Fujii, Hirosane Fukui, Akihiko Hamada, Ryusei Hirao, Yuki Silva, Stela Ishitani Itow, Yoshitaka Kirikawa, Rintaro Koshimoto, Naoki Matsubara, Yutaka Miyazaki, Shota Muraki, Yasushi Olmschenk, Greg Ranc, Clément Rattenbury, Nicholas J. Satoh, Yuki Suzuki, Daisuke Tomoyoshi, Mio Tristram, Paul J. Vandorou, Aikaterini Yama, Hibiki Yamashita, Kansuke Department of Astronomy Tsinghua University Beijing China Solar Stellar and Planetary Physics Division Center for Astrophysics Harvard and Smithsonian Cambridge MA USA Optical Astronomy Division Korea Astronomy and Space Science Institute Daejeon South Korea Department of Astronomy and Space Science National University of Science and Technology Daejeon South Korea Department of Astronomy Westlake University Hangzhou China Astronomical Observatory University of Warsaw Warszawa Poland Department of Earth and Space Science Graduate School of Science Osaka University Osaka Japan Galaxies and Cosmology Max-Planck-Institute for Astronomy Heidelberg Germany Department of Astronomy Ohio State University Columbus OH United States Department of Physics and Astronomy University of Canterbury Christchurch New Zealand Department of Physics Chungbuk National University Cheongju South Korea Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot Israel School of Space Research Kyung Hee University South Korea Center for Large Telescopes Korea Astronomy and Space Science Institute Daejeon South Korea Center for Cosmology and AstroParticle Physics Ohio State University Columbus OH United States Department of Engineering Physics Tsinghua University Beijing China Astronomy Department Harvard University Cambridge MA United States Department of Physics University of Warwick Coventry United Kingdom Department of Astrophysics and Planetary Sciences Villanova University Villanova PA United States Institute for Space-Earth Environmental Research Nagoya University Nagoya Japan Exoplanets and Stellar Astrophysics Laboratory NASA Goddard Space Flight Center Greenbelt MD United States Department of Astronomy University of Maryland College Park MD United States Institute of Natural and Mathematical Sciences Massey University Auckland New Zealand Department of Earth and Planetary Science Graduate School of Science University of Tokyo

Exoplanets classified as super-Earths are commonly observed on short-period orbits, close to their host stars, but their abundance on wider orbits is poorly constrained. Gravitational microlensing is sensitive to exoplanets on wide orbits. We observed the microlensing event OGLE-2016-BLG-0007, which indicates an exoplanet with a planet-to-star mass ratio roughly double the Earth-Sun mass ratio, on an orbit longer than Saturn's. We combined this event with a larger sample from a microlensing survey to determine the distribution of mass ratios for planets on wide orbits. We infer that there are ~0.35 super-Earth planets per star on Jupiter-like orbits. The observations are most consistent with a bimodal distribution, with separate peaks for super-Earths and gas giants. We suggest that this reflects differences in their formation processes.

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Improving efficiency of the path optimization method for a gauge theory

引用

Physical Review D 2023年第3期107卷 034509-034509页

作者： Yusuke Namekawa Kouji Kashiwa Hidefumi Matsuda Akira Ohnishi Hayato Takase Education and Research Center for Artificial Intelligence and Data Innovation Hiroshima University Hiroshima 730-0053 Japan Department of Physics Faculty of Science Kyoto University Kyoto 606-8502 Japan Yukawa Institute for Theoretical Physics Kyoto University Kyoto 606-8502 Japan Department of Computer Science and Engineering Faculty of Information Engineering Fukuoka Institute of Technology Fukuoka 811-0295 Japan Department of Physics and Center for Field Theory and Particle Physics Fudan University Shanghai 200433 China

We investigate efficiency of a gauge-covariant neural network and an approximation of the Jacobian in optimizing the complexified integration path toward evading the sign problem in lattice field theories. For the construction of the complexified integration path, we employ the path optimization method. The two-dimensional U(1) gauge theory with the complex gauge-coupling constant is used as a laboratory to evaluate the efficiency. It is found that the gauge-covariant neural network, which is composed of the Stout-like smearing, can enhance the average phase factor, as the gauge-invariant input does. For the approximation of the Jacobian, we test the most drastic case in which we perfectly drop the Jacobian during the learning process. It reduces the numerical cost of the Jacobian calculation from O(N3) to O(1), where N means the number of degrees of freedom of the theory. The path optimization using this Jacobian approximation still enhances the average phase factor at expense of a slight increase of the statistical error.

关键词： Lattice gauge theory Machine learning

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Searching for neutrino signals correlated with LHAASO diffuse Galactic emission 38

Searching for neutrino signals correlated with LHAASO diffus...

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Li, Wenlian Huang, Tian-Qi Xu, Donglian He, Huihai Cao, Zhen Aharonian, F. An, Q. Axikegu Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Cai, J.T. Cao, Q. Cao, W.Y. Cao, Zhe Chang, J. Chang, J.F. Chen, A.M. Chen, E.S. Chen, Liang Chen, Lin Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. 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. Cui, Y.D. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu della Volpe, D. Dong, X.Q. Duan, K.K. Fan, J.H. Fan, Y.Z. Fang, J. Fang, K. Feng, C.F. Feng, L. Feng, S.H. Feng, X.T. Feng, Y.L. Gabici, S. Gao, B. Gao, C.D. Gao, L.Q. 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. He, H.H. He, H.N. He, J.Y. He, X.B. He, Y. Heller, M. Hor, Y.K. 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. Huang, Z.C. Ji, X.L. Jia, H.Y. Jia, K. Jiang, K. Jiang, X.W. Jiang, Z.J. Jin, M. Kang, M.M. Ke, T. Kuleshov, D. Kurinov, K. Li, B.B. Li, Cheng Li, Cong Li, D. Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, Jian Li, Jie Li, K. 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, H. Liu, H.D. Liu, J. Liu, J.L. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Lu, R. Luo, Q. 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, Z.W. Pang, B.Y. Pattarakijwanich, P. Pei, Z.Y. Qi, M.Y. Qi, Y.Q. Qiao, B.Q. Qin, J.J. Ruffolo, D. Sáiz, A. Semikoz, D. Shao, C.Y. Shao, L. Shchegolev, O. Sheng, X.D. Shu, F.W. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai201210 China Key Laboratory of Particle Astrophysics Experimental Physics Division Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Key Laboratory of Particle Astrophyics 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 Sichuan Chengdu610000 China Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Max-Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg69029 Germany State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Anhui Hefei230026 China School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Sichuan Chengdu610031 China School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210023 China Center for Astrophysics Guangzhou University Guangdong Guangzhou510006 China Hebei Normal University Hebei Shijiazhuang050024 China Key Laboratory of Dark Matter and Space Astronomy Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Tsung-Dao Lee Institute School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Key Laboratory of Cosmic Rays Tibet University Ministry of Education Tibet Lhasa850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Physics and Astronomy Sun Yat-sen University Zhuhai519000 China School of Physics Sun Ya

The diffuse Galactic γ-ray emission is produced from the interaction of cosmic rays and interstellar medium or radiation fields in the Galaxy, where neutrino production is also expected. Recently, the Large High Altitude Air Shower Observatory (LHAASO) reported the measurements of the diffuse γ-ray from the Galactic plane with energies above 10 TeV. In this study, we construct the neutrino emission template based on LHAASO’s observation and search for diffuse neutrinos accompanying the LHAASO diffuse Galactic γ-ray emission using ten-year IceCube track events. No significant signals are found. We set 90% confidence level upper limits, resulting in the neutrino flux of dν/dEν = 1.27 × 10−14(Eν/25TeV)−2.99TeV−1cm−2s−1 for the diffuse γ-ray flux map with a 1.5σ significance cut. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Gamma rays

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Electromagnetic field in a cavity induced by gravitational waves

arXiv

引用

arXiv 2023年

作者： Ahn, Danho Bae, Yeong-Bok Im, Sang Hui Park, Chan Center for Axion and Precision Physics Research Institute for Basic Science Daejeon34051 Korea Republic of Department of Physics Chung-Ang University Seoul06974 Korea Republic of Particle Theory and Cosmology Group Center for Theoretical Physics of the Universe Institute for Basic Science Daejeon34051 Korea Republic of Center for the Gravitational-Wave Universe Astronomy Program Department of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of Institute for Gravitational Wave Astronomy Henan Academy of Sciences Henan Zhengzhou450046 China

The detection method of gravitational waves (GW) using electromagnetic (EM) cavities has garnered significant attention in recent years. This paper thoroughly examines the analysis for the perturbation of the EM field and raises some issues in the existing literature. Our work demonstrates that the rigidity condition imposed on the material, as provided in the literature, is inappropriate due to its reliance on a gauge-dependent quantity that cannot be controlled experimentally. Instead, we incorporate elasticity into the material and revise the governing equations for the electric field induced by GWs, expressing them solely in terms of gauge-invariant quantities. Applying these equations to cylindrical cavities, we present the GW antenna patterns for the detector. Copyright © 2023, The Authors. All rights reserved.

关键词： Directional patterns (antenna)

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First Indication of Solar B8 Neutrinos through Coherent Elastic Neutrino-Nucleus Scattering in PandaX-4T

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Physical Review Letters 2024年第19期133卷 191001页

作者： Zihao Bo Wei Chen Xun Chen Yunhua Chen Zhaokan Cheng Xiangyi Cui Yingjie Fan Deqing Fang Zhixing Gao Lisheng Geng Karl Giboni Xunan Guo Xuyuan Guo Zichao Guo Chencheng Han Ke Han Changda He Jinrong He Di Huang Houqi Huang Junting Huang Ruquan Hou Yu Hou Xiangdong Ji Xiangpan Ji Yonglin Ju Chenxiang Li Jiafu Li Mingchuan Li Shuaijie Li Tao Li Zhiyuan Li Qing Lin Jianglai Liu Congcong Lu Xiaoying Lu Lingyin Luo Yunyang Luo Wenbo Ma Yugang Ma Yajun Mao Yue Meng Xuyang Ning Binyu Pang Ningchun Qi Zhicheng Qian Xiangxiang Ren Dong Shan Xiaofeng Shang Xiyuan Shao Guofang Shen Manbin Shen Wenliang Sun Yi Tao Anqing Wang Guanbo Wang Hao Wang Jiamin Wang Lei Wang Meng Wang Qiuhong Wang Shaobo Wang Siguang Wang Wei Wang Xiuli Wang Xu Wang Zhou Wang Yuehuan Wei Weihao Wu Yuan Wu Mengjiao Xiao Xiang Xiao Kaizhi Xiong Yifan Xu Shunyu Yao Binbin Yan Xiyu Yan Yong Yang Peihua Ye Chunxu Yu Ying Yuan Zhe Yuan Youhui Yun Xinning Zeng Minzhen Zhang Peng Zhang Shibo Zhang Shu Zhang Tao Zhang Wei Zhang Yang Zhang Yingxin Zhang Yuanyuan Zhang Li Zhao Jifang Zhou Jiaxu Zhou Jiayi Zhou Ning Zhou Xiaopeng Zhou Yubo Zhou Zhizhen Zhou School of Physics and Astronomy Shanghai Jiao Tong University Key Laboratory for Particle Astrophysics and Cosmology (MoE) Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai 200240 China New Cornerstone Science Laboratory Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai 201210 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu 610213 China Jinping Deep Underground Frontier Science and Dark Matter Key Laboratory of Sichuan Province Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu 610051 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai 519082 China Department of Physics Yantai University Yantai 264005 China Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) Institute of Modern Physics Fudan University Shanghai 200433 China School of Physics Beihang University Beijing 102206 China Peng Huanwu Collaborative Center for Research and Education Beihang University Beijing 100191 China International Research Center for Nuclei and Particles in the Cosmos & Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing 100191 China Southern Center for Nuclear-Science Theory (SCNT) Institute of Modern Physics Chinese Academy of Sciences Huizhou 516000 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai 200240 China School of Mechanical Engineering Shanghai Jiao Tong University Shanghai 200240 China Department of Physics University of Maryland College Park Maryland 20742 USA School of Physics Nankai University Tianjin 300071 China School of Physics Sun Yat-Sen University Guangzhou 510275 China State Key Laboratory of Particle Detection and Electronics Department of Modern Physics Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Qingdao 266237 China Key Laboratory of Particle Physics and Particle

The PandaX-4T liquid xenon detector at the China Jinping Underground Laboratory is used to measure the solar B8 neutrino flux by detecting neutrinos through coherent scattering with xenon nuclei. data samples requiring the coincidence of scintillation and ionization signals (paired), as well as unpaired ionization-only signals (US2), are selected with energy threshold of approximately 1.1 keV (0.33 keV) nuclear recoil energy. Combining the commissioning run and the first science run of PandaX-4T, a total exposure of 1.20 and 1.04 tonne·year are collected for the paired and US2, respectively. After unblinding, 3 and 332 events are observed with an expectation of 2.8±0.5 and 251±32 background events, for the paired and US2 data, respectively. A combined analysis yields a best-fit B8 neutrino signal of 3.5 (75) events from the paired (US2) data sample, with ∼37% uncertainty, and the background-only hypothesis is disfavored at 2.64σ significance. This gives a solar B8 neutrino flux of (8.4±3.1)×106 cm−2 s−1, consistent with the standard solar model prediction. It is also the first indication of solar B8 neutrino “fog” in a dark matter direct detection experiment.

关键词： Nucleus-neutrino interactions particle dark matter Solar neutrinos Neutrino detection Time-projection chambers

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A complete analysis of inflation with piecewise quadratic potential

arXiv

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arXiv 2024年

作者： Wang, Xinpeng Ma, Xiao-Han Sasaki, Misao The University of Tokyo Institutes for Advanced Study The University of Tokyo Chiba277-8583 Japan School of Physics Science and Engineering Tongji University Shanghai200092 China Deep Space Exploration Laboratory School of Physical Sciences University of Science and Technology of China Anhui Hefei230026 China CAS Key Laboratory for Researches in Galaxies and Cosmology Department of Astronomy School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan

We conduct a thorough study of the comoving curvature perturbation R in single-field inflation with two stages, represented by a piecewise quadratic potential, where both the first and second derivatives are allowed to be discontinuous at the transition point. We calculate the evolution of R by combining the perturbative and non-perturbative methods consistently, and obtain the power spectrum and the non-Gaussian features in the probability distribution function. We find that both the spectrum and the statistics of R depend significantly on the second derivatives of the potential at both the first and second stages. Furthermore, we find a new parameter constructed from the potential parameters, which we call α, plays a decisive role in determining various features in the spectrum such as the amplitude, the slope, and the existence of a dip. In particular, we recover the typical k4 growth of the spectrum in most cases, but the maximum growth rate of k5(log k)2 can be obtained by fine-tuning the parameters. Then, using the δN formalism valid on superhorizon scales, we give fully nonlinear formulas for R in terms of the scalar field perturbation δ and its time derivative. In passing, we point out the importance of the nonlinear evolution of δ on superhorizon scales. Finally, using the Press-Schechter formalism for simplicity, we discuss the effect of the non-Gaussian tails of the probability distribution function on the primordial black hole formation. Copyright © 2024, The Authors. All rights reserved.

关键词： Distribution functions

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Searching for neutrino emission from the Cygnus region 38

Searching for neutrino emission from the Cygnus region

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38th International Cosmic Ray Conference, ICRC 2023

The Cygnus region, which contains massive molecular and atomic clouds and young stars, is a promising Galactic neutrino source candidate. Cosmic rays transport in the region can produce neutrinos and γ-rays. Using ten years of track events detected by the IceCube Neutrino Observatory, we conduct searches for neutrino signals from the Cygnus region with a template method. Four templates, including the CO template, HI template, uniform template, and 2D Gaussian template, are used in this study. No significant emissions are found. We set upper limits for each template, with the resulting upper limit for the CO template being dν/dEν = 6.25 × 10−17(Eν/100TeV)−3TeV−1cm−2s−1 © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： cosmology

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Detected stochastic gravitational waves and subsolar-mass primordial black holes

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Physical Review D 2024年第6期109卷 063506-063506页

作者： Keisuke Inomata Kazunori Kohri Takahiro Terada Kavli Institute for Cosmological Physics The University of Chicago Chicago Illinois 60637 USA Division of Science National Astronomical Observatory of Japan (NAOJ) and SOKENDAI 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Theory Center IPNS and QUP (WPI) KEK 1-1 Oho Tsukuba Ibaraki 305-0801 Japan Kavli IPMU (WPI) UTIAS The University of Tokyo Kashiwa Chiba 277-8583 Japan Particle Theory and Cosmology Group Center for Theoretical Physics of the Universe Institute for Basic Science (IBS) Daejeon 34126 Korea

Multiple pulsar timing array (PTA) collaborations recently announced the evidence of common-spectral processes caused by gravitational waves (GWs). These can be the stochastic GW background and its origin may be astrophysical and/or cosmological. We interpret it as the GWs induced by the primordial curvature perturbations and discuss their implications on primordial black holes (PBHs). We show that the newly released data suggest PBHs much lighter than the Sun [O(10−4)M⊙ for the delta-function curvature spectrum; data releases.

关键词： Classical black holes cosmology Gravitational waves Perturbation theory

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

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Physical Review D 2024年第5期109卷 055008-055008页

作者： Amit Adhikary Shankha Banerjee Rahool Kumar Barman Brian Batell Biplob Bhattacherjee Camellia Bose Zhuoni Qian Michael Spannowsky Institute of Theoretical Physics Faculty of Physics University of Warsaw Pasteura 5 PL 02-093 Warsaw Poland Centre for High Energy Physics Indian Institute of Science Bangalore 560012 India CERN Theoretical Physics Department CH-1211 Geneva 23 Switzerland Department of Physics Oklahoma State University Stillwater Oklahoma 74078 USA Pittsburgh Particle Physics Astrophysics and Cosmology Center Department of Physics and Astronomy University of Pittsburgh Pittsburgh 15260 USA Hangzhou Normal University Hangzhou Zhejiang 311121 China Institute for Particle Physics Phenomenology Durham University South Road Durham DH1 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.

关键词： Extensions of Higgs sector particle phenomena Phenomenology Higgs bosons Tau leptons

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The IXPE view of GRB 221009A 38

The IXPE view of GRB 221009A

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38th International Cosmic Ray Conference, ICRC 2023

作者： Di Lalla, Niccolò Negro, Michela Omodei, Nicola Veres, Peter Silvestri, Stefano Manfreda, Alberto Burns, Eric W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States University of Maryland Baltimore County BaltimoreMD21250 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 Department of Space Science University of Alabama HuntsvilleAL35899 United States Center for Space Plasma and Aeronomic Research University of Alabama HuntsvilleAL35899 United States Istituto Nazionale di Fisica Nucleare Sezione di Pisa Pisa56127 Italy Università di Pisa Dipartimento di Fisica Enrico Fermi Pisa56127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Napoli Napoli80126 Italy Department of Physics and Astronomy Louisiana State University Baton RougeLA70803 United States

GRB 221009A is an exceptionally bright gamma-ray burst (GRB) that reached Earth on October 9th, 2022 after traveling through the dust of the Milky Way. The Imaging X-ray Polarimetry Explorer (IXPE) pointed at GRB 221009A on October 11th and measured, for the first time, the 2-8 keV X-ray polarization of both a GRB afterglow and rings of dust-scattered photons which are echoes of the GRB prompt emission. We set upper limits to the polarization degree of the afterglow and the prompt emission of respectively 13.8% and 55% at a 99% confidence level, providing constraints on the jet opening angle of the GRB and other properties of the emitting region. In this contribution, I present on behalf on the IXPE Collaboration the results of the analysis and interpretation of the IXPE observation of GRB 221009A. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Gamma rays

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