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arXiv 2022年

作者： Yao, Fei Walter, Lisa Chen, Jiunn-Wei Hua, Jun Ji, Xiangdong Jin, Luchang Lahrtz, Sebastian Ma, Lingquan Mohanta, Protick Schäfer, Andreas Shu, Hai-Tao Su, Yushan Sun, Peng Xiong, Xiaonu Yang, Yi-Bo Zhang, Jian-Hui School of Physics and Electronics Central South University Changsha418003 China Center of Advanced Quantum Studies Department of Physics Beijing Normal University Beijing100875 China Institut für Theoretische Physik Universität Regensburg RegensburgD-93040 Germany Department of Physics Center for Theoretical Physics Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan Physics Division National Center for Theoretical Sciences Taipei10617 Taiwan Guangdong Provincial Key Laboratory of Nuclear Science Institute of Quantum Matter South China Normal University Guangzhou510006 China Guangdong-Hong Kong Joint Laboratory of Quantum Matter Southern Nuclear Science Computing Center South China Normal University Guangzhou510006 China Department of Physics University of Maryland College ParkMD20742 United States Physics Department University of Connecticut StorrsCT06269-3046 United States RIKEN BNL Research Center Brookhaven National Laboratory UptonNY11973 United States School of Physical Sciences National Institute of Science Education and Research HBNI Odisha752050 India Institute of Modern Physics Chinese Academy of Sciences Gansu Province Lanzhou730000 China Department of Physics Institute of Theoretical Physics Nanjing Normal University Jiangsu Nanjing210023 China CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing100190 China School of Fundamental Physics and Mathematical Sciences Hangzhou Institute for Advanced Study UCAS Hangzhou310024 China International Centre for Theoretical Physics Asia-Pacific Hangzhou Beijing China University of Chinese Academy of Sciences School of Physical Sciences Beijing100049 China

We report a state-of-the-art lattice QCD calculation of the isovector quark transversity distribution of the proton in the continuum and physical mass limit using large-momentum effective theory. The calculation is done at four lattice spacings a = {0.098, 0.085, 0.064, 0.049} fm and various pion masses ranging between 220 and 350 MeV, with proton momenta up to 2.8 GeV. The result is non-perturbatively renormalized in the hybrid scheme with self renormalization which treats the infrared physics at large correlation distance properly, and extrapolated to the continuum, physical mass and infinite momentum limit. We also compare with recent global analyses for the nucleon isovector quark transversity distribution. Copyright © 2022, The Authors. All rights reserved.

关键词： Quantum theory

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A study of analysis method for the identification of UHECR source type 37

A study of analysis method for the identification of UHECR s...

引用

37th International Cosmic Ray Conference, ICRC 2021

作者： Yoshida, Fugo Tameda, Yuichiro Abbasi, R.U. Abu-Zayyad, T. Allen, M. Arai, Y. Arimura, R. Barcikowski, E. Belz, J.W. Bergman, D.R. Blake, S.A. Buckland, I. Cady, R. Cheon, B.G. Chiba, J. Chikawa, M. Fujii, T. Fujisue, K. Fujita, K. Fujiwara, R. Fukushima, M. Fukushima, R. Furlich, G. Gonzalez, R. Hanlon, W. Hayashi, M. Hayashida, N. Hibino, K. Higuchi, R. Honda, K. Ikeda, D. Inadomi, T. Inoue, N. Ishii, T. Ito, H. Ivanov, D. Iwakura, H. Iwasaki, A. Jeong, H.M. Jeong, S. Jui, C.C.H. Kadota, K. Kakimoto, F. Kalashev, O. Kasahara, K. Kasami, S. Kawai, H. Kawakami, S. Kawana, S. Kawata, K. Kharuk, I. Kido, E. Kim, H.B. Kim, J.H. Kim, J.H. Kim, M.H. Kim, S.W. Kimura, Y. Kishigami, S. Kubota, Y. Kurisu, S. Kuznetsov, M. Kwon, Y.J. Lee, K.H. Lubsandorzhiev, B. Lundquist, J.P. Machida, K. Matsumiya, H. Matsuyama, T. Matthews, J.N. Mayta, R. Minamino, M. Mukai, K. Myers, I. Nagataki, S. Nakai, K. Nakamura, R. Nakamura, T. Nakamura, T. Nakamura, Y. Nakazawa, A. Nishio, E. Nonaka, T. Oda, H. Ogio, S. Ohnishi, M. Ohoka, H. Oku, Y. Okuda, T. Omura, Y. Ono, M. Onogi, R. Oshima, A. Ozawa, S. Park, I.H. Potts, M. Pshirkov, M.S. Remington, J. Rodriguez, D.C. Rubtsov, G.I. Ryu, D. Sagawa, H. Sahara, R. Saito, Y. Sakaki, N. Sako, T. Sakurai, N. Sano, K. Sato, K. Seki, T. Sekino, K. Shah, P.D. Shibasaki, Y. Shibata, F. Shibata, N. Shibata, T. Shimodaira, H. Shin, B.K. Shin, H.S. Shinto, D. Smith, J.D. Sokolsky, P. Sone, N. Stokes, B.T. Stroman, T.A. Takagi, Y. Takahashi, Y. Takamura, M. Takeda, M. Takeishi, R. Taketa, A. Takita, M. Tameda, Y. Tanaka, H. Tanaka, K. Tanaka, M. Tanoue, Y. Thomas, S.B. Thomson, G.B. Tinyakov, P. Tkachev, I. Tokuno, H. Tomida, T. Troitsky, S. Tsuda, R. Tsunesada, Y. Uchihori, Y. Udo, S. Uehama, T. Urban, F. Wong, T. Yada, K. Yamamoto, M. Yamazaki, K. Yang, J. Yashiro, K. Yoshida, F. Yoshioka, Y. Zhezher, Y. Zundel, Z. Department of Engineering Science Faculty of Engineering Osaka Electro-Communication University 18-8 Hatsucho Neyagawa-shi Osaka Japan Department of Physics Loyola University Chicago ChicagoIL United States High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT United States Graduate School of Science Osaka City University Osaka Osaka Japan Department of Physics The Research Institute of Natural Science Hanyang University Seongdong-gu Seoul Korea Republic of Department of Physics Tokyo University of Science Chiba Noda Japan Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa Japan The Hakubi Center for Advanced Research Graduate School of Science Kyoto University Kitashirakawa-Oiwakecho Sakyo-ku Kyoto Japan Information Engineering Graduate School of Science and Technology Shinshu University Nagano Nagano Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama Japan Interdisciplinary Graduate School of Medicine and Engineering University of Yamanashi Yamanashi Kofu Japan Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano Japan The Graduate School of Science and Engineering Saitama University Saitama Saitama Japan Astrophysical Big Bang Laboratory RIKEN Saitama Wako Japan Department of Physics SungKyunKwan University Jang-an-gu Suwon Korea Republic of Department of Physics Tokyo City University Setagaya-ku Tokyo Japan Institute for Nuclear Research The Russian Academy of Sciences Moscow Russia Faculty of Systems Engineering and Science Shibaura Institute of Technology Minato-ku Tokyo Japan Department of Engineering Science Faculty of Engineering Osaka Electro-Communication University Neyagawa-shi Osaka Japan Department of Physics Chiba University Chiba Chiba Japan Service de Physique Théorique Université Libre de Bruxelles Brussels Belgium Department of Physics Yonsei University Seodaemu

The autocorrelation analysis using the arrival direction of Ultra High Energy Cosmic Rays (UHECRs) has been previously reported by the Telescope Array (TA) experiment. It is expected that the autocorrelation function reflects the source distribution. We simulate the expected arrival direction distribution of the cosmic rays using the catalogs of candidate sources. We take into account random deflection in the magnetic fields, with the magnitude of deflection determined by the charge and energy of the cosmic rays, coherence length and magnitude of the extragalactic magnetic field (EGMF), and by distance to source. In addition, in order to compare with the results of TA, we consider the TA exposure. We compare the autocorrelation of the arrival directions corresponding to different source catalogs with the isotropic distribution. We calculate the autocorrelation function for each type of source candidates using this procedure. We will discuss the ability of this method to identify the source type of UHECRs. © Copyright owned by the author(s).

关键词： Cosmic rays

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Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA

引用

Radiation Detection Technology and Methods 2021年第4期5卷 531-541页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang X.C.Chan B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen X.L.Chen Y.Chen N.Chen Y.D.Chen S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.D’Ettorre Piazzoli X.J.Don J.H.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fan C.F.Feng L.Feng S.H.Fen Y.L.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge L.S.Gen G.H.Gong Q.B.Gou M.H.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu S.Hu S.C.Hu X.J.Hu D.H.Huang Q.L.Huan W.H.Huang X.T.Huang Z.C.Huang F.Ji X.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li W.L.Li X.Li X.Li X.R.Li Y.Li Y.Z.Li Z.Li Z.Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu H.Liu H.D.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev X.D.Shen J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun Z.B.Sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wan C.Wang H.Wang H.G.Wang J.C.Wang J.S.Wang L.P.Wang L.Y.Wan R.N.Wang W.Wang W.Wang X.G.Wang X.J.Wan X.Y.Wang Y.D.Wan Y.J.Wan Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu S.Wu W.X.Wu X.F.Wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao H.B.Xiao G.G.Xin Y.L.Xin Y.Xing D.L.Xu R.X.Xu L.Xue D.H.Yan C.W.Yang F.F.Yang J.Y.Yang L.L.Yang M.J.Yan R.Z.Yang S.B.Yang Y.H.Yao Z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.W.Zhang L.Zhang L.Zhang L.X.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhan X.Zhang X.P.Zhan Y.Zhan Y.Zhang Y.F.Zhang Y.L.Zhan B.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou X.X.Zhou C.G. Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physic

Purpose Observation of high energy and very high emission from Gamma Ray Bursts(GRBs)is crucial to study the gigantic explosion and the underline *** a large field-of-view and almost full duty cycle,the Water Cherenkov Detector Array(WCDA),a sub-array of the Large High Altitude Air Shower Observatory(LHAASO),is appropriate to monitor the very high energy emission from unpredictable transients such as *** Nevertheless,the main issue for an extensive air shower array is the high energy threshold which limits the horizon of the *** address this issue a new trigger method is developed in this article to lower the energy threshold of WCDA for GRB *** The proposed method significantly improves the detection efficiency of WCDA for gamma-rays around the GRB direction at 10-300 *** sensitivity of the WCDA for GRB detection with the new trigger method is *** achieved sensitivity of the quarter WCDA array above 10 GeV is comparable with that of *** data analysis process and corresponding fluence upper limit for GRB 190719C is presented as an example.

关键词： LHAASO WCDA GRB

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Search for light dark matter with ionization signals in the PandaX-4T Experiment

arXiv

引用

arXiv 2022年

作者： Li, Shuaijie Wu, Mengmeng Abdukerim, Abdusalam Bo, Zihao Chen, Wei Chen, Xun Chen, Yunhua Cheng, Chen Cheng, Zhaokan Cui, Xiangyi Fan, Yingjie Fang, Deqing Fu, Changbo Fu, Mengting Geng, Lisheng Giboni, Karl Gu, Linhui Guo, Xuyuan Han, Chencheng Han, Ke He, Changda He, Jinrong Huang, Di Huang, Yanlin Huang, Zhou Hou, Ruquan Ji, Xiangdong Ju, Yonglin Li, Chenxiang Li, Jiafu Li, Mingchuan Li, Shu Lin, Qing Liu, Jianglai Lu, Xiaoying Luo, Lingyin Luo, Yunyang Ma, Wenbo Ma, Yugang Mao, Yajun Meng, Yue Ning, Xuyang Qi, Ningchun Qian, Zhicheng Ren, Xiangxiang Shaheed, Nasir Shang, Changsong Shang, Xiaofeng Shen, Guofang Si, Lin Sun, Wenliang Tan, Andi Tao, Yi Wang, Anqing Wang, Meng Wang, Qiuhong Wang, Shaobo Wang, Siguang Wang, Wei Wang, Xiuli Wang, Zhou Wei, Yuehuan Wu, Weihao Xia, Jingkai Xiao, Mengjiao Xiao, Xiang Xie, Pengwei Yan, Binbin Yan, Xiyu Yang, Jijun Yang, Yong Yao, Yukun You, Zhengyun Yu, Chunxu Yuan, Jumin Yuan, Ying Yuan, Zhe Zeng, Xinning Zhang, Dan Zhang, Minzhen Zhang, Peng Zhang, Shibo Zhang, Shu Zhang, Tao Zhang, Yang Zhang, Yingxin Zhang, Yuanyuan Zhao, Li Zheng, Qibin Zhou, Jifang Zhou, Ning Zhou, Xiaopeng Zhou, Yong Zhou, Yubo Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai200240 China School of Physics Sun Yat-Sen University Guangzhou510275 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu610213 China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu610051 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai519082 China School of Physics Nankai University Tianjin300071 China Institute of Modern Physics Fudan University Shanghai200433 China School of Physics Peking University Beijing100871 China School of Physics Beihang University Beijing102206 China International Research Center for Nuclei and Particles in the Cosmos Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing100191 China School of Physics and Microelectronics Zhengzhou University Henan Zhengzhou450001 China School of Medical Instrument and Food Engineering University of Shanghai for Science and Technology Shanghai200093 China Department of Physics University of Maryland College ParkMD20742 United States School of Mechanical Engineering Shanghai Jiao Tong University Shanghai200240 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei230026 China Department of Modern Physics University of Science and Technology of China Hefei230026 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Shandong Qingdao266237 China Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong University Shandong Qingdao266237 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai200240 China School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China

We report the search results of light dark matter through its interactions with shell electrons and nuclei, using the commissioning data from the PandaX-4T liquid xenon detector. Low energy events are selected to have an ionization-only signal between 60 to 200 photoelectrons, corresponding to a mean nuclear recoil energy from 0.77 to 2.54 keV and electronic recoil energy from 0.07 to 0.23 keV. With an effective exposure of 0.55 tonne·year, we set the most stringent limits within a mass range from 40 MeV/c2 to 10 GeV/c2 for point-like dark matter-electron interaction, 100 MeV/c2 to 10 GeV/c2 for dark matter-electron interaction via a light mediator, and 3.2 to 4 GeV/c2 for dark matter-nucleon spin-independent interaction. For DM interaction with electrons, our limits are closing in on the parameter space predicted by the freeze-in and freeze-out mechanisms in the early Universe. © 2022, CC BY.

关键词： Germanium alloys

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Searching for gravitational-wave signals from precessing black hole binaries with the GstLAL pipeline

arXiv

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arXiv 2024年

作者： Schmidt, Stefano Caudill, Sarah Creighton, Jolien D.E. Magee, Ryan Tsukada, Leo Adhicary, Shomik Baral, Pratyusava Baylor, Amanda Cannon, Kipp Cousins, Bryce Ewing, Becca Fong, Heather George, Richard N. Godwin, Patrick Hanna, Chad Harada, Reiko Huang, Yun-Jing Huxford, Rachael Joshi, Prathamesh Kennington, James Kuwahara, Soichiro Li, Alvin K.Y. Meacher, Duncan Messick, Cody Morisaki, Soichiro Mukherjee, Debnandini Niu, Wanting Pace, Alex Posnansky, Cort Ray, Anarya Sachdev, Surabhi Sakon, Shio Singh, Divya Tapia, Ron Tsutsui, Takuya Ueno, Koh Viets, Aaron Wade, Leslie Wade, Madeline Nikhef Science Park 105 Amsterdam1098 XG Netherlands Utrecht University Princetonplein 1 Utrecht3584 CC Netherlands Department of Physics University of Massachusetts DartmouthMA02747 United States Center for Scientific Computing and Data Science Research University of Massachusetts DartmouthMA02747 United States Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee MilwaukeeWI53201 United States LIGO Laboratory California Institute of Technology PasadenaCA91125 United States Department of Physics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States RESCEU The University of Tokyo Tokyo113-0033 Japan Department of Physics University of Illinois UrbanaIL61801 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada Graduate School of Science The University of Tokyo Tokyo113-0033 Japan Center for Gravitational Physics University of Texas at Austin AustinTX78712 United States LIGO Laboratory California Institute of Technology MS 100-36 PasadenaCA91125 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan NASA Marshall Space Flight Center HuntsvilleAL35811 United States Center for Space Plasma and Aeronomic Research University of Alabama in Huntsville HuntsvilleAL35899 United States School of Physics Georgia Institute of Technology AtlantaGA30332 United States Concordia University

Precession in Binary Black Holes (BBH) is caused by the failure of the Black Hole spins to be aligned and its study can open up new perspectives in gravitational waves (GW) astronomy, providing, among other advancements, a precise measure of distance and an accurate characterization of the BBH spins. However, detecting precessing signals is a highly non-trivial task, as standard matched filtering pipelines for GW searches are built on many assumptions that do not hold in the precessing case. This work details the upgrades made to the GstLAL pipeline to facilitate the search for precessing BBH signals. The implemented changes in the search statistics and in the signal consistency test are then described in detail. The performance of the upgraded pipeline is evaluated through two extensive searches of precessing signals, targeting two different regions in the mass space, and the consistency of the results is examined. Additionally, the benefits of the upgrades are assessed by comparing the sensitive volume of the precessing searches with two corresponding traditional aligned-spin searches. While no significant sensitivity improvement is observed for precessing binaries with mass ratio q 6, a volume increase of up to 100% is attainable for heavily asymmetric systems with largely misaligned spins. Furthermore, our findings suggest that the primary cause of degraded performance in an aligned-spin search targeting precessing signals is not a poor signal-to-noise-ratio recovery but rather the failure of the ξ2 signal-consistency test. Our work paves the way for a large-scale search for precessing signals, which could potentially result in exciting future detections. © 2024, CC BY.

关键词： Matched filters

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Exploring asymmetric substructures of the outer disk based on the conjugate angle of the radial action

arXiv

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arXiv 2023年

作者： Xu, Y. Liu, C. Li, Z. Tian, H. Bird, Sarah A. Newberg, H.J. Shao, S. Deng, L.C. CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University 800 Dongchuan Road Shanghai200240 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China College of Science China Three Gorges University Yichang443002 China Center for Astronomy and Space Sciences China Three Gorges University Yichang443002 China Department of Physics Applied Physics and Astronomy Rensselaer Polytechnic Institute TroyNY12180 United States Key Laboratory for Computational Astrophysics National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China

We use the conjugate angle of radial action (θR), the best representation of the orbital phase, to explore the "mid-plane, north branch, south branch" and "Monoceros area" disk structures that were previously revealed in the LAMOST K giants (Xu et al. 2020). The former three substructures, identified by their 3D kinematical distributions, have been shown to be projections of the phase space spiral (resulting from nonequilibrium phase mixing). In this work, we find that all of these substructures associated with the phase spiral show high aggregation in conjugate angle phase space, indicating that the clumping in conjugate angle space is a feature of ongoing, incomplete phase mixing. We do not find the Z−VZ phase spiral located in the "Monoceros area", but we do find a very highly concentrated substructure in the quadrant of conjugate angle space with the orbital phase from the apocenter to the guiding radius. The existence of the clump in conjugate angle space provides a complementary way to connect the "Monoceros area" with the direct response to a perturbation from a significant gravitationally interactive event. Using test particle simulations, we show that these features are analogous to disturbances caused by the impact of the last passage of the Sagittarius dwarf spheroidal galaxy. © 2023, CC BY.

关键词： Galaxies

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Hints of dark photon dark matter from observations and hydrodynamical simulations of the low-redshift Lyman-α forest

arXiv

引用

arXiv 2022年

作者： Bolton, James S. Caputo, Andrea Liu, Hongwan Viel, Matteo School of Physics and Astronomy University of Nottingham University Park NottinghamNG7 2RD United Kingdom School of Physics and Astronomy Tel-Aviv University Tel-Aviv69978 Israel Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot7610001 Israel Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY10003 United States Department of Physics Princeton University Princeton NJ08544 United States SISSA - International School for Advanced Studies Via Bonomea 265 TriesteI-34136 Italy IFPU Institute for Fundamental Physics of the Universe Via Beirut 2 TriesteI-34151 Italy INFN Sezione di Trieste Via Valerio 2 TriesteI-34127 Italy INAF - Osservatorio Astronomico di Trieste Via G. B. Tiepolo 11 TriesteI-34143 Italy

Recent work has suggested that an additional 6.9 eV per baryon of heating in the intergalactic medium is needed to reconcile hydrodynamical simulations with Lyman-α forest absorption line widths at redshift z 0.1. Resonant conversion of dark photon dark matter into low frequency photons is a viable source of such heating. We perform the first hydrodynamical simulations including dark photon heating and show that dark photons with mass mA' ∼ 8 × 10−14 eV c−2 and kinetic mixing ϵ ∼ 5 × 10−15 can alleviate the heating excess. A prediction of this model is a non-standard thermal history for underdense gas at z 3. Copyright © 2022, The Authors. All rights reserved.

关键词： Photons

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Gravitational wave signatures from reheating in Chern-Simons running-vacuum cosmology

arXiv

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arXiv 2024年

作者： Tzerefos, Charalampos Papanikolaou, Theodoros Basilakos, Spyros Saridakis, Emmanuel N. Mavromatos, Nick E. Department of Physics National & Kapodistrian University of Athens Zografou Campus AthensGR 157 73 Greece National Observatory of Athens Lofos Nymfon Athens11852 Greece Scuola Superiore Meridionale Largo S. Marcellino 10 Napoli80138 Italy Sezione di Napoli Via Cinthia 21 Napoli80126 Italy Academy of Athens Research Center for Astronomy and Applied Mathematics Soranou Efesiou 4 Athens11527 Greece School of Sciences European University Cyprus Diogenes Street Engomi Nicosia1516 Cyprus CAS Key Laboratory for Researches in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China Departamento de Matemáticas Universidad Católica del Norte Avda. Angamos 0610 Casilla 1280 Antofagasta Chile Physics Division School of Applied Mathematical and Physical Sciences National Technical University of Athens Zografou Campus Athens157 80 Greece Theoretical Particle Physics and Cosmology group Department of Physics King’s College London LondonWC2R 2LS United Kingdom

Within the context of a Chern-Simons running-vacuum-model (RVM) cosmology, one expects an early-matter dominated (eMD) reheating period after RVM inflation driven by the axion field. Treating thus in this work Chern-Simons RVM cosmology as an effective f(R) gravity theory characterized by logarithmic corrections of the spacetime curvature, we study the gravitational-wave (GW) signal induced by the nearly-scale invariant inflationary adiabatic curvature perturbations during the transition from the eMD era driven by the axion to the late radiation-dominated era. Remarkably, by accounting for the extra GW scalaron polarization present within f(R) gravity theories, we find regions in the parameter space of the theory where one is met with a distinctive induced GW signal with a universal f6 high-frequency scaling compared to the f7 scaling present in general relativity (GR). Interestingly enough, for axion masses ma higher than 1 GeV and axion gauge couplings fa above 10−3MPl, one can produce induced GW spectra within the sensitivity bands of future GW observatories such as the Einstein Telescope (ET), the Laser Interferometer Space Antenna (LISA), the Big Bang Observer (BBO) and the Square Kilometer Arrays (SKA). © 2024, CC BY.

关键词： cosmology

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Study of e ⁺ e ⁻ → γϕJ/ψ from √s = 4.600 to 4.951 GeV

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Journal of High Energy physics 2023年第1期2023卷 132页

作者： Ablikim, M. Achasov, M.N. Adlarson, P. Albrecht, M. Aliberti, R. Amoroso, A. An, M.R. An, Q. Bai, Y. Bakina, O. Baldini Ferroli, R. Balossino, I. Ban, Y. Batozskaya, V. Becker, D. Begzsuren, K. Berger, N. Bertani, M. Bettoni, D. Bianchi, F. Bianco, E. Bloms, J. Bortone, A. Boyko, I. Briere, R.A. Brueggemann, A. Cai, H. Cai, X. Calcaterra, A. Cao, G.F. Cao, N. Cetin, S.A. Chang, J.F. Chang, W.L. Che, G.R. Chelkov, G. Chen, Chao Chen, G. Chen, H.S. Chen, M.L. Chen, S.J. Chen, S.M. Chen, T. Chen, X.R. Chen, X.T. Chen, Y.B. Chen, Z.J. Cheng, W.S. Choi, S.K. Chu, X. Cibinetto, G. Cossio, F. Cui, J.J. Dai, H.L. Dai, J.P. Dbeyssi, A. de Boer, R.E. Dedovich, D. Deng, Z.Y. Denig, A. Denysenko, I. Destefanis, M. De Mori, F. Ding, Y. Dong, J. Dong, L.Y. Dong, M.Y. Dong, X. Du, S.X. Duan, Z.H. Egorov, P. Fan, Y.L. Fang, J. Fang, S.S. Fang, W.X. Fang, Y. Farinelli, R. Fava, L. Feldbauer, F. Felici, G. Feng, C.Q. Feng, J.H. Fischer, K. Fritsch, M. Fritzsch, C. Fu, C.D. Gao, H. Gao, Y.N. Gao, Yang Garbolino, S. Garzia, I. Ge, P.T. Ge, Z.W. Geng, C. Gersabeck, E.M. Gilman, A. Goetzen, K. Gong, L. Gong, W.X. Gradl, W. Greco, M. Gu, L.M. Gu, M.H. Gu, Y.T. Guan, C.Y. Guo, A.Q. Guo, L.B. Guo, R.P. Guo, Y.P. Guskov, A. Han, W.Y. Hao, X.Q. Harris, F.A. He, K.K. He, K.L. Heinsius, F.H. Heinz, C.H. Heng, Y.K. Herold, C. Hou, G.Y. Hou, Y.R. Hou, Z.L. Hu, H.M. Hu, J.F. Hu, T. Hu, Y. Huang, G.S. Huang, K.X. Huang, L.Q. Huang, X.T. Huang, Y.P. Huang, Z. Hussain, T. Hüsken, N. Imoehl, W. Irshad, M. Jackson, J. Jaeger, S. Janchiv, S. Jang, E. Jeong, J.H. Ji, Q. Ji, Q.P. Ji, X.B. Ji, X.L. Ji, Y.Y. Jia, Z.K. Jiang, P.C. Jiang, S.S. Jiang, X.S. Jiang, Y. Jiao, J.B. Jiao, Z. Jin, S. Jin, Y. Jing, M.Q. Johansson, T. Kabana, S. Kalantar-Nayestanaki, N. Kang, X.L. Kang, X.S. Kappert, R. Kavatsyuk, M. Ke, B.C. Keshk, I.K. Khoukaz, A. Kiuchi, R. Kliemt, R. Koch, L. Kolcu, O.B. Kopf, B. Kuemmel, M. Kuessner, M. Kupsc, A. Kühn, W. Lane, J.J. Lange, J.S. Larin, P. Lavania, A. Lavezzi, L. Lei, T.T. Lei, Z.H. Leithoff, H. Lellmann, M. Lenz, T. Li, Cheng Li Institute of High Energy Physics Beijing 100049 China Beihang University Beijing 100191 China Beijing Institute of Petrochemical Technology Beijing 102617 China Bochum Ruhr-University Bochum D-44780 Germany Carnegie Mellon University Pittsburgh 15213 PA United States Central China Normal University Wuhan 430079 China Central South University Changsha 410083 China China Center of Advanced Science and Technology Beijing 100190 China China University of Geosciences Wuhan 430074 China COMSATS University Islamabad Lahore Campus Defence Road Off Raiwind Road Lahore 54000 Pakistan Fudan University Shanghai 200433 China G.I. Budker Institute of Nuclear Physics SB RAS (BINP) Novosibirsk 630090 Russian Federation GSI Helmholtzcentre for Heavy Ion Research GmbH Darmstadt D-64291 Germany Guangxi Normal University Guilin 541004 China Guangxi University Nanning 530004 China Hangzhou Normal University Hangzhou 310036 China Hebei University Baoding 071002 China Helmholtz Institute Mainz Staudinger Weg 18 Mainz D-55099 Germany Henan Normal University Xinxiang 453007 China Henan University of Science and Technology Luoyang 471003 China Henan University of Technology Zhengzhou 450001 China Huangshan College Huangshan 245000 China Hunan Normal University Changsha 410081 China Hunan University Changsha 410082 China Indian Institute of Technology Madras Chennai 600036 India Indiana University Bloomington 47405 IN United States INFN Laboratori Nazionali di Frascati Frascati I-00044 Italy INFN Sezione di Perugia Perugia I-06100 Italy University of Perugia Perugia I-06100 Italy INFN Sezione di Ferrara Ferrara I-44122 Italy University of Ferrara Ferrara I-44122 Italy Institute of Modern Physics Lanzhou 730000 China Institute of Physics and Technology Peace Avenue 54B Ulaanbaatar 13330 Mongolia Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica Chile Jilin University Changchun 130012 China Johannes Gutenber

Using data samples with an integrated luminosity of 6.4 fb−1 collected by the BESIII detector operating at the BEPCII storage ring, the process of e+e− → γϕJ/ψ is studied. The processes of e+e− → ϕχc1,c2, χc1,c2... 详细信息

Using data samples with an integrated luminosity of 6.4 fb⁻¹ collected by the BESIII detector operating at the BEPCII storage ring, the process of e⁺e⁻ → γϕJ/ψ is studied. The processes of e⁺e⁻ → ϕχ_c1,_c2, χ_c1,_c2 → γJ/ψ are observed with a significance of more than 10σ. The s-dependent cross section of e⁺e⁻ → ϕχ_c1,_c2 is measured between 4.600 and 4.951 GeV, and evidence of a resonance structure is found for the first time in the ϕχ_c2 process. We also search for the processes of e⁺e⁻ → γX(4140), γX(4274) and γX(4500) via the γϕJ/ψ final state, but no obvious structures are found. The upper limits on the production cross section times the branching fraction for these processes at the 90% confidence level are reported. [Figure not available: see fulltext.]. © 2023, The Author(s).

关键词： e+-e− Experiments Exotics Quarkonium Spectroscopy

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

arXiv

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arXiv 2024年

作者： Hanna, Chad Kennington, James Niu, Wanting Sakon, Shio Singh, Divya Adhicary, Shomik Baral, Pratyusava Baylor, Amanda Cannon, Kipp Caudill, Sarah Cousins, Bryce Creighton, Jolien D.E. Ewing, Becca Fong, Heather George, Richard N. Godwin, Patrick Harada, Reiko Huang, Yun-Jing Huxford, Rachael Joshi, Prathamesh Kuwahara, Soichiro Li, Alvin K.Y. Magee, Ryan Meacher, Duncan Messick, Cody Morisaki, Soichiro Mukherjee, Debnandini Pace, Alexander Posnansky, Cort Ray, Anarya Sachdev, Surabhi Schmidt, Stefano Shah, Urja Tapia, Ron Tsukada, Leo Ueno, Koh Viets, Aaron Wade, Leslie Wade, Madeline Yarbrough, Zach Zhang, Noah Department of Physics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Department of Physics University of California BerkeleyCA94720 United States Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee MilwaukeeWI53201 United States RESCEU The University of Tokyo Tokyo113-0033 Japan Department of Physics University of Massachusetts DartmouthMA02747 United States Center for Scientific Computing and Data Science Research University of Massachusetts DartmouthMA02747 United States Department of Physics University of Illinois UrbanaIL61801 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada Graduate School of Science The University of Tokyo Tokyo113-0033 Japan Center for Gravitational Physics University of Texas at Austin AustinTX78712 United States LIGO Laboratory California Institute of Technology MS 100-36 PasadenaCA91125 United States LIGO Laboratory California Institute of Technology PasadenaCA91125 United States MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan NASA Marshall Space Flight Center HuntsvilleAL35811 United States Center for Space Plasma and Aeronomic Research University of Alabama in Huntsville HuntsvilleAL35899 United States Center of Interdisciplinary Education and Research in Astrophysics Northwestern University IL60201 United States School of Physics Georgia Insti

Matched-filtering searches for gravitational-wave signals from compact binary mergers employ template banks which are a collection of modeled waveforms described by unique intrinsic parameters. We present two banks designed for low-latency and archive sub-solar mass (SSM) searches in data from the fourth observing run of LIGO-Virgo-KAGRA, and demonstrate the efficacy of the banks via simulated signals. Further, we introduce a set of modifications to the geometric, manifold algorithm [1, 2] that allow the method to work for exceedingly low component masses necessary for SSM bank production. The archive search bank contains a total of 3,452,006 templates, and covers a mass parameter space of 0.2 to 10 M☉ in the larger component and 0.2 to 1.0 M☉ in the smaller component, the spin parameter space of −0.9 to 0.9 for masses above 0.5 M☉ and −0.1 to 0.1 for masses below 0.5 M☉, and the mass ratio parameter space of 1 to 10. The PSD used was from a week of the first half of the fourth observing run of Advanced LIGO, Advanced Virgo, and KAGRA, and the low frequency cutoff was set to 45 Hz with a maximum waveform duration of 128 seconds. The bank simulations performed using SBank have shown that the banks presented in this paper have sufficient efficacy for use in their respective searches. Copyright © 2024, The Authors. All rights reserved.

关键词： Gravity waves

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