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arXiv 2024年

作者： Phurailatpam, Hemantakumar More, Anupreeta Narola, Harsh Yin, Ng Chung Janquart, Justin Van Den Broeck, Chris Hannuksela, Otto Akseli Singh, Neha Keitel, David Department of Physics The Chinese University of Hong Kong Shatin New Territories Hong Kong Post Bag 4 Ganeshkhind Pune411007 India 5-1-5 Kashiwanoha Kashiwa-shi Chiba277-8583 Japan Department of Physics Utrecht University Princetonplein 1 Utrecht3584 CC Netherlands Nikhef – National Institute for Subatomic Physics Science Park Amsterdam1098 XG Netherlands Center for Cosmology Particle Physics and Phenomenology - CP3 Universit'e Catholique de Louvain Louvain-La-Neuve B-1348 Belgium Royal Observatory of Belgium Avenue Circulaire 3 Uccle1180 Belgium Departament de Física Universitat de les Illes Balears IAC3-IEEC Crta. Valldemossa km 7.5 PalmaE-07122 Spain

Gravitational waves (GWs) are ripples in the fabric of space and time caused by the acceleration of unevenly distributed mass or masses. Observable GWs are created especially during the violent cosmic events of merging compact binaries, such as ‘binary black holes’ (BBHs), ‘binary neutron stars’ (BNSs), and ‘neutron star and black hole pair’ (NSBHs). GWs emitted by these events can be distorted or magnified by the gravitational fields of massive objects such as galaxies or galaxy clusters, a phenomenon known as gravitational lensing. Profound comprehension of gravitational lensing’s impact on GW signals is imperative to their accurate interpretation and the extraction of astrophysical insights therein. For this purpose, statistical modelling of GWs lensing can provide valuable insights into the properties of the lensing objects and GW sources. Such statistics require accurate and efficient means to calculate the detectable lensing rates, which depend on up-to-date modeling and implementation of lens and source properties and their distribution. The outcomes of these computational analyses not only contribute to generating dependable forecasts but also play an important role in validating forthcoming lensing events (Janquart et al. 2023) (Collaboration et al. 2023) (Abbott et al. 2021). Obtaining precise outcomes in statistical analyses of this nature necessitates the utilization of large-scale sampling, often numbering in the millions. However, this process is computationally demanding. The ler framework addresses this by employing innovative techniques to optimize the workflow and computation efficiency required for handling large-scale statistical analyses, essential for modeling detectable events and calculating rates. Its integration of modular statistical components enhances the framework’s adaptability and extendability, thus proving to be an invaluable asset in the evolving field of gravitational wave research. Detailed description, source code, and examples

关键词： Gravity waves

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A search for the ultra high energy neutrinos with the low threshold phased array trigger system of the Askaryan Radio Array

arXiv

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arXiv 2024年

作者： Dasgupta, Paramita Ali, S. Allison, P. Archambault, S. Beatty, J.J. Besson, D.Z. Bishop, A. Chen, P. Chen, Y.C. Chen, Y.-C. Clark, B.A. Connolly, A. Couberly, K. Cremonesi, L. Cummings, A. Dasgupta, P. Debolt, R. de Kockere, S. de Vries, K.D. Deaconu, C. DuVernois, M.A. Flaherty, J. Friedman, E. Gaior, R. Giri, P. Hanson, J. Harty, N. Hoffman, K.D. Huang, M.H. Hughes, K. Ishihara, A. Karle, A. Kelley, J.L. Kim, K.-C. Kim, M.-C. Kravchenko, I. Krebs, R. Kuo, C.Y. Kurusu, K. Latif, U.A. Liu, C.H. Liu, T.C. Luszczak, W. Mase, K. Muzio, M.S. Nam, J. Nichol, R.J. Novikov, A. Nozdrina, A. Oberla, E. Pan, Y. Pfendner, C. Punsuebsay, N. Roth, J. Salcedo-Gomez, A. Seckel, D. Seikh, M.F.H. Shiao, Y.-S. Su, S.C. Toscano, S. Torres, J. Touart, J. van Eijndhoven, N. Varner, G.S. Vieregg, A. Wang, M.-Z. Wang, S.-H. Wissel, S.A. Xie, C. Yoshida, S. Young, R. Dept. of Physics and Astronomy University of Kansas LawrenceKS66045 United States Dept. of Physics Center for Cosmology and AstroParticle Physics The Ohio State University ColumbusOH43210 United States Dept. of Physics Chiba University Chiba Japan Dept. of Physics University of Wisconsin-Madison MadisonWI53706 United States Dept. of Physics Grad. Inst. of Astrophys. Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei Taiwan Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Physics and Astronomy University College London London United Kingdom Center for Multi-Messenger Astrophysics Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Dept. of Physics Pennsylvania State University University ParkPA16802 United States Dept. of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Vrije Universiteit Brussel Brussels Belgium Dept. of Physics Enrico Fermi Institue Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Dept. of Physics and Astronomy University of Nebraska LincolnNE68588 United States Dept. Physics and Astronomy Whittier College WhittierCA90602 United States Dept. of Physics University of Delaware NewarkDE19716 United States Dept. of Energy Engineering National United University Miaoli Taiwan Dept. of Applied Physics National Pingtung University Pingtung County Pingtung City900393 Taiwan Dept. of Physics and Astronomy Denison University GranvilleOH43023 United States National Nano Device Laboratories Hsinchu300 Taiwan Universite Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dept. of Physics and Astronomy University of Hawaii ManoaHI96822 United States

The Askaryan Radio Array (ARA) is an in-ice ultra high energy (UHE, > 10 PeV) neutrino experiment at the South Pole that aims to detect UHE neutrino-induced radio emission in ice. ARA consists of five independent stations each consisting of a cubical lattice of in-ice antenna clusters with a side length of ∼10 m buried at ∼200 m below the ice surface. The fifth station of ARA (A5) is special as this station has an additional central string, the phased array (PA), which provides an interferometric trigger that enables ARA to trigger on weak signals that are otherwise buried in noise. Leveraging the low threshold phased array trigger, ARA was the first radio neutrino experiment to demonstrate significant improvement in sensitivity to weak signals. In this contribution, we present initial results from a neutrino search combining information from both the traditional station antennas and the phased array antennas of the A5 station. We show the improved vertex reconstruction achieved with this approach, and leveraging this improvement, we expect to enhance the analysis efficiency beyond what has been achieved previously by ARA. This analysis is the paradigmatic representation of future neutrino searches with the next generation of in-ice neutrino experiments. Copyright © 2024, The Authors. All rights reserved.

关键词： Antenna phased arrays

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Search for high-mass Wγ and Zγ resonances using hadronic W/Z boson decays from 139 fb⁻¹ of pp collisions at √s = 13 TeV with the ATLAS detector

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Journal of High Energy physics 2023年第7期2023卷 1-47页

作者： Aad, G. Abbott, B. Abbott, D.C. Abed Abud, A. Abeling, K. Abhayasinghe, D.K. Abidi, S.H. Aboulhorma, A. Abramowicz, H. Abreu, H. Abulaiti, Y. Abusleme Hoffman, A.C. Acharya, B.S. Achkar, B. Adam, L. Adam Bourdarios, C. Adamczyk, L. Adamek, L. Addepalli, S.V. Adelman, J. Adiguzel, A. Adorni, S. Adye, T. Affolder, A.A. Afik, Y. Agapopoulou, C. Agaras, M.N. Agarwala, J. Aggarwal, A. Agheorghiesei, C. Aguilar-Saavedra, J.A. Ahmad, A. Ahmadov, F. Ahmed, W.S. Ai, X. Aielli, G. Aizenberg, I. Akatsuka, S. Akbiyik, M. Åkesson, T.P.A. Akimov, A.V. Al Khoury, K. Alberghi, G.L. Albert, J. Albicocco, P. Alconada Verzini, M.J. Alderweireldt, S. Aleksa, M. Aleksandrov, I.N. Alexa, C. Alexopoulos, T. Alfonsi, A. Alfonsi, F. Alhroob, M. Ali, B. Ali, S. Aliev, M. Alimonti, G. Allaire, C. Allbrooke, B.M.M. Allport, P.P. Aloisio, A. Alonso, F. Alpigiani, C. Alunno Camelia, E. Alvarez Estevez, M. Alviggi, M.G. Amaral Coutinho, Y. Ambler, A. Ambroz, L. Amelung, C. Amidei, D. Amor Dos Santos, S.P. Amoroso, S. Amos, K.R. Amrouche, C.S. Ananiev, V. Anastopoulos, C. Andari, N. Andeen, T. Anders, J.K. Andrean, S.Y. Andreazza, A. Angelidakis, S. Angerami, A. Anisenkov, A.V. Annovi, A. Antel, C. Anthony, M.T. Antipov, E. Antonelli, M. Antrim, D.J.A. Anulli, F. Aoki, M. Aparisi Pozo, J.A. Aparo, M.A. Aperio Bella, L. Aranzabal, N. Araujo Ferraz, V. Arcangeletti, C. Arce, A.T.H. Arena, E. Arguin, J.-F. Argyropoulos, S. Arling, J.-H. Armbruster, A.J. Armstrong, A. Arnaez, O. Arnold, H. Arrubarrena Tame, Z.P. Artoni, G. Asada, H. Asai, K. Asai, S. Asbah, N.A. Asimakopoulou, E.M. Asquith, L. Assahsah, J. Assamagan, K. Astalos, R. Atkin, R.J. Atkinson, M. Atlay, N.B. Atmani, H. Atmasiddha, P.A. Augsten, K. Auricchio, S. Austrup, V.A. Avner, G. Avolio, G. Ayoub, M.K. Azuelos, G. Babal, D. Bachacou, H. Bachas, K. Bachiu, A. Backman, F. Badea, A. Bagnaia, P. Bahrasemani, H. Bailey, A.J. Bailey, V.R. Baines, J.T. Bakalis, C. Baker, O.K. Bakker, P.J. Bakos, E. Bakshi Gupta, D. Balaji, S. Balasubramanian, R. Baldin, E.M. Balek, P. Ballabene, E. Balli, F Department of Physics University of Adelaide Adelaide Australia Department of Physics University of Alberta Edmonton AB Canada Department of Physics Ankara University Ankara Turkey Division of Physics TOBB University of Economics and Technology Ankara Turkey LAPP Université Savoie Mont Blanc CNRS/IN2P3 Annecy France High Energy Physics Division Argonne National Laboratory Argonne IL United States Department of Physics University of Arizona Tucson AZ United States Department of Physics University of Texas at Arlington Arlington TX United States Physics Department National and Kapodistrian University of Athens Athens Greece Physics Department National Technical University of Athens Zografou Greece Department of Physics University of Texas at Austin Austin TX United States Bahcesehir University Faculty of Engineering and Natural Sciences Istanbul Turkey Istanbul Bilgi University Faculty of Engineering and Natural Sciences Istanbul Turkey Department of Physics Bogazici University Istanbul Turkey Department of Physics Engineering Gaziantep University Gaziantep Turkey Institut de Física d’Altes Energies (IFAE) Barcelona Institute of Science and Technology Barcelona Spain Institute of High Energy Physics Chinese Academy of Sciences Beijing China Physics Department Tsinghua University Beijing China Department of Physics Nanjing University Nanjing China University of Chinese Academy of Science (UCAS) Beijing China Institute of Physics University of Belgrade Belgrade Serbia Department for Physics and Technology University of Bergen Bergen Norway Physics Division Lawrence Berkeley National Laboratory Berkeley CA United States Institut für Physik Humboldt Universität zu Berlin Berlin Germany Albert Einstein Center for Fundamental Physics and Laboratory for High Energy Physics University of Bern Bern Switzerland School of Physics and Astronomy University of Birmingham Birmingham United Kingdom Facultad de Ciencias y Centro de Investigaciónes

A search for high-mass charged and neutral bosons decaying to Wγ and Zγ final states is presented in this paper. The analysis uses a data sample of s = 13 TeV proton-proton collisions with an integrated luminosity of 139 fb⁻¹ collected by the ATLAS detector during LHC Run 2 operation. The sensitivity of the search is determined using models of the production and decay of spin-1 charged bosons and spin-0/2 neutral bosons. The range of resonance masses explored extends from 1.0 TeV to 6.8 TeV. At these high resonance masses, it is beneficial to target the hadronic decays of the W and Z bosons because of their large branching fractions. The decay products of the high-momentum W/Z bosons are strongly collimated and boosted-boson tagging techniques are employed to improve the sensitivity. No evidence of a signal above the Standard Model backgrounds is observed, and upper limits on the production cross-sections of these bosons times their branching fractions to Wγ and Zγ are derived for various boson production models. [Figure not available: see fulltext.]. © 2023, The Author(s).

关键词： Hadron-Hadron Scattering

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Measurement of Electron Antineutrino Oscillation Amplitude and Frequency via Neutron Capture on Hydrogen at Daya Bay

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Physical Review Letters 2024年第15期133卷 151801页

作者： F. P. An W. D. Bai A. B. Balantekin M. Bishai S. Blyth G. F. Cao J. Cao J. F. Chang Y. Chang H. S. Chen H. Y. Chen S. M. Chen Y. Chen Y. X. Chen Z. Y. Chen J. Cheng Y.-C. Cheng Z. K. Cheng J. J. Cherwinka M. C. Chu J. P. Cummings O. Dalager F. S. Deng X. Y. Ding Y. Y. Ding M. V. Diwan T. Dohnal D. Dolzhikov J. Dove K. V. Dugas H. Y. Duyang D. A. Dwyer J. P. Gallo M. Gonchar G. H. Gong H. Gong W. Q. Gu J. Y. Guo L. Guo X. H. Guo Y. H. Guo Z. Guo R. W. Hackenburg Y. Han S. Hans M. He K. M. Heeger Y. K. Heng Y. K. Hor Y. B. Hsiung B. Z. Hu J. R. Hu T. Hu Z. J. Hu H. X. Huang J. H. Huang X. T. Huang Y. B. Huang P. Huber D. E. Jaffe K. L. Jen X. L. Ji X. P. Ji R. A. Johnson D. Jones L. Kang S. H. Kettell S. Kohn M. Kramer T. J. Langford J. Lee J. H. C. Lee R. T. Lei R. Leitner J. K. C. Leung F. Li H. L. Li J. J. Li Q. J. Li R. H. Li S. Li S. C. Li W. D. Li X. N. Li X. Q. Li Y. F. Li Z. B. Li H. Liang C. J. Lin G. L. Lin S. Lin J. J. Ling J. M. Link L. Littenberg B. R. Littlejohn J. C. Liu J. L. Liu J. X. Liu C. Lu H. Q. Lu K. B. Luk B. Z. Ma X. B. Ma X. Y. Ma Y. Q. Ma R. C. Mandujano C. Marshall K. T. McDonald R. D. McKeown Y. Meng J. Napolitano D. Naumov E. Naumova T. M. T. Nguyen J. P. Ochoa-Ricoux A. Olshevskiy J. Park S. Patton J. C. Peng C. S. J. Pun F. Z. Qi M. Qi X. Qian N. Raper J. Ren C. Morales Reveco R. Rosero B. Roskovec X. C. Ruan B. Russell H. Steiner J. L. Sun T. Tmej K. Treskov W.-H. Tse C. E. Tull Y. C. Tung B. Viren V. Vorobel C. H. Wang J. Wang M. Wang N. Y. Wang R. G. Wang W. Wang X. Wang Y. F. Wang Z. Wang Z. M. Wang H. Y. Wei L. H. Wei W. Wei L. J. Wen K. Whisnant C. G. White H. L. H. Wong E. Worcester D. R. Wu Q. Wu W. J. Wu D. M. Xia Z. Q. Xie Z. Z. Xing H. K. Xu J. L. Xu T. Xu T. Xue C. G. Yang L. Yang Y. Z. Yang H. F. Yao M. Ye M. Yeh B. L. Young H. Z. Yu Z. Y. Yu B. B. Yue V. Zavadskyi S. Zeng Y. Zeng L. Zhan C. Zhang F. Y. Zhang H. H. Zhang J. L. Zhang J. W. Zhang Q. M. Zhang S. Q. Zhang X. T. Zhang Y. M. Zhang Y. X. Zhang Y. Y. Zhang Z. J. Zhang Z. P. Zhang Z. Y. Zhang J. Zhao R. Z. Zhao L Sun Yat-Sen (Zhongshan) University Guangzhou University of Wisconsin Madison Wisconsin 53706 Brookhaven National Laboratory Upton New York 11973 Department of Physics National Taiwan University Taipei Institute of High Energy Physics Beijing New Cornerstone Science Laboratory Institute of High Energy Physics Beijing National United University Miao-Li Department of Engineering Physics Shenzhen University Shenzhen North China Electric Power University Beijing Chinese University of Hong Kong Hong Kong Siena College Loudonville New York 12211 Department of Physics and Astronomy University of California Irvine California 92697 University of Science and Technology of China Hefei Shandong University Jinan Charles University Faculty of Mathematics and Physics Prague Joint Institute for Nuclear Research Dubna Moscow Region Department of Physics University of Illinois at Urbana-Champaign Urbana Illinois 61801 Lawrence Berkeley National Laboratory Berkeley California 94720 Department of Physics Illinois Institute of Technology Chicago Illinois 60616 Beijing Normal University Beijing Department of Nuclear Science and Technology School of Energy and Power Engineering Xi’an Jiaotong University Xi’an Wright Laboratory and Department of Physics Yale University New Haven Connecticut 06520 China Institute of Atomic Energy Beijing Guangxi University No. 100 Daxue East Road Nanning Center for Neutrino Physics Virginia Tech Blacksburg Virginia 24061 Institute of Physics National Chiao-Tung University Hsinchu Department of Physics University of Cincinnati Cincinnati Ohio 45221 Department of Physics College of Science and Technology Temple University Philadelphia Pennsylvania 19122 Dongguan University of Technology Dongguan Department of Physics University of California Berkeley California 94720 Department of Physics The University of Hong Kong Pokfulam Hong Kong School of Physics Nankai University Tianjin Department of Physics and Astronomy Shanghai Jiao Tong University

This Letter reports the first measurement of the oscillation amplitude and frequency of reactor antineutrinos at Daya Bay via neutron capture on hydrogen using 1958 days of data. With over 3.6 million signal candidates, an optimized candidate selection, improved treatment of backgrounds and efficiencies, refined energy calibration, and an energy response model for the capture-on-hydrogen sensitive region, the relative ν¯e rates and energy spectra variation among the near and far detectors gives sin22θ13=0.0759−0.0049+0.0050 and Δm322=(2.72−0.15+0.14)×10−3 eV2 assuming the normal neutrino mass ordering, and Δm322=(−2.83−0.14+0.15)×10−3 eV2 for the inverted neutrino mass ordering. This estimate of sin22θ13 is consistent with and essentially independent from the one obtained using the capture-on-gadolinium sample at Daya Bay. The combination of these two results yields sin22θ13=0.0833±0.0022, which represents an 8% relative improvement in precision regarding the Daya Bay full 3158-day capture-on-gadolinium result.

关键词： Neutrino mixing Neutrino oscillations Neutrinos Neutrino detection particle mixing & oscillations Scintillators

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Measurement of Double Beta Decay Half-life of 136Xe with the PandaX-4T Detector

arXiv

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arXiv 2022年

作者： Si, Lin Cheng, Zhaokan Abdukerim, Abdusalam Bo, Zihao Chen, Wei Chen, Xun Chen, Yunhua Cheng, Chen Cheng, Yunshan Cui, Xiangyi Fan, Yingjie Fang, Deqing Fu, Changbo Fu, Mengting Geng, Lisheng Giboni, Karl Gu, Linhui Guo, Xuyuan 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 Li, Shuaijie Lin, Qing Liu, Jianglai Lu, Xiaoying Luo, Lingyin Luo, Yunyang Ma, Wenbo Ma, Yugang Mao, Yajun Meng, Yue Shaheed, Nasir Shang, Xiaofeng Ning, Xuyang Qi, Ningchun Qian, Zhicheng Ren, Xiangxiang Shang, Changsong Shen, Guofang 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, Mengmeng Wu, Weihao Xia, Jingkai Xiao, Mengjiao Xiao, Xiang Xie, Pengwei Yan, Binbin Yan, Xiyu Yang, Jijun Yang, Yong Yu, Chunxu Yuan, Jumin Yuan, Ying Yuan, Zhe Zhang, Dan Zhang, Minzhen Zhang, Peng Zhang, Shibo Zhang, Shu Zhang, Tao Zhao, Li Zheng, Qibin Zhou, Jifang Zhou, Ning Zhou, Xiaopeng Zhou, Yong School of Physics and Astronomy Shanghai Jiao Tong University MOE Key Laboratory for Particle Astrophysics and Cosmology Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai519082 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu610213 China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu610051 China School of Physics Sun Yat-Sen University Guangzhou510275 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 Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai200240 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 Beijing100191 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 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 SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai200240 China

Precise measurement of two-neutrino double beta decay (DBD) half-life is an important step for the searches of Majorana neutrinos with neutrinoless double beta decay. We report the measurement of DBD half-life of 136Xe using the PandaX-4T dual-phase Time Projection Chamber (TPC) with 3.7-tonne natural xenon and the first 94.9-day physics data release. The background model in the fiducial volume is well constrained in situ by events in the outer active region. With a 136Xe exposure of 15.5 kg-year, we establish the half-life as 2.27 ± 0.03(stat.) ± 0.10(syst.) × 1021 years. This is the first DBD half-life measurement with natural xenon and demonstrates the physics capability of a large-scale liquid xenon TPC in the field of rare event searches. Copyright © 2022, The Authors. All rights reserved.

关键词： particle detectors

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Search for Light Dark Matter–Electron Scattering in the PandaX-II Experiment

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Physical Review Letters 2021年第21期126卷 211803-211803页

作者： Chen Cheng Pengwei Xie Abdusalam Abdukerim Wei Chen Xun Chen Yunhua Chen Xiangyi Cui Yingjie Fan Deqing Fang Changbo Fu Mengting Fu Lisheng Geng Karl Giboni Linhui Gu Xuyuan Guo Ke Han Changda He Shengming He Di Huang Yan Huang Yanlin Huang Zhou Huang Xiangdong Ji Yonglin Ju Shuaijie Li Qing Lin Huaxuan Liu Jianglai Liu Liqiang Liu Xiaoying Lu Wenbo Ma Yugang Ma Yajun Mao Yue Meng Parinya Namwongsa Kaixiang Ni Jinhua Ning Xuyang Ning Xiangxiang Ren Nasir Shaheed Changsong Shang Guofang Shen Lin Si Andi Tan Anqing Wang Hongwei Wang Meng Wang Qiuhong Wang Siguang Wang Wei Wang Xiuli Wang Zhou Wang Mengmeng Wu Shiyong Wu Weihao Wu Jingkai Xia Mengjiao Xiao Xiang Xiao Binbin Yan Jijun Yang Yong Yang Chunxu Yu Jumin Yuan Ying Yuan Xinning Zeng Dan Zhang Tao Zhang Li Zhao Qibin Zheng Jifang Zhou Ning Zhou Xiaopeng Zhou School of Physics Sun Yat-Sen University Guangzhou 510275 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai 200240 China 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 Shanghai Jiao Tong University Sichuan Research Institute Chengdu 610213 China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu 610051 China School of Physics Nankai University Tianjin 300071 China Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) Institute of Modern Physics Fudan University Shanghai 200433 China School of Physics Peking University Beijing 100871 China School of Physics 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 School of Medical Instrument and Food Engineering University of Shanghai for Science and Technology Shanghai 200093 China Department of Physics University of Maryland College Park Maryland 20742 USA School of Mechanical Engineering Shanghai Jiao Tong University Shanghai 200240 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei 230026 China Department of Modern Physics University of Science and Technology of China Hefei 230026 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Qingdao 266237 Shandong China Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong University Qingdao 266237 Shandong China Shanghai Advanced Research Institute Chinese Academy of Sciences Shanghai 201210 China

We report constraints on light dark matter through its interactions with shell electrons in the PandaX-II liquid xenon detector with a total 46.9 tonnes/day exposure. To effectively search for these very low energy electron recoils, ionization-only signals are selected from the data. 1821 candidates are identified within an ionization signal range between 50 and 75 photoelectrons, corresponding to a mean electronic recoil energy from 0.08 to 0.15 keV. The 90% C.L. exclusion limit on the scattering cross section between the dark matter and electron is calculated with systematic uncertainties properly taken into account. Under the assumption of point interaction, we provide the world’s most stringent limit within the dark matter mass range from 15 to 30 MeV/c2, with the corresponding cross section from 2.5×10−37 to 3.1×10−38 cm2.

关键词： Dark matter particle dark matter Dark matter detectors

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The prolific thermonuclear X-ray bursts from the outburst of the newly discovered millisecond pulsar MAXI J1816–195 observed by Insight-HXMT and NICER

arXiv

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arXiv 2022年

作者： Chen, Yu-Peng Zhang, Shu Ji, Long Zhang, Shuang-Nan Wang, Peng-Ju Kong, Ling-Da Chang, Zhi Peng, Jing-Qiang Shui, Qing-Cang Li, Jian Tao, Lian Ge, Ming-Yu Qu, Jin-Lu Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100049 China Institut für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Sand 1 TübingenD-72076 Germany CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China

MAXI J1816–195 is a newly discovered accreting millisecond pulsar with prolific thermonuclear bursts, detected during its outburst in 2022 June by Insight-HXMT and NICER. During the outburst, Insight-HXMT detected 73 bursts in its peak and decay phase, serving as a prolific burst system found in the accreting millisecond pulsars. By analyzing one burst which was simultaneously detected by Insight-HXMT and NICER, we find a mild deviation from the conventional blackbody model. By stacking the Insight-HXMT lightcurves of 66 bursts which have similar profiles and intensities, a hard X-ray shortage is detected with a significance of 15.7 σ in 30–100 keV. The shortage is about 30% of the persistent flux, which is low compared with other bursters. The shortage fraction is energy-dependent: larger in a higher energy band. These findings make the newly discovered millisecond MAXI J1816-195 a rather peculiar system compared with other millisecond pulsars and atoll bursters. In addition, based on the brightest burst, we derive an upper limit of the distance as 6.3 kpc, and therefore estimate the upper limit of the inner disc radius of the accretion disc to be ∼ 40 km. Assuming the radius as the magnetospheric radius, the derived magnetic field strength is about 7.1×108 G. © 2022, CC BY.

关键词： Magnetosphere

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Dwarf-Dwarf Interactions Can Both Trigger and Quench Star Formation

arXiv

引用

arXiv 2023年

作者： Kado-Fong, Erin Robinson, Azia Nyland, Kristina Greene, Jenny E. Suess, Katherine A. Stierwalt, Sabrina Beaton, Rachael Physics Department Yale Center for Astronomy & Astrophysics PO Box 208120 New HavenCT06520 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08540 United States U.S. Naval Research Laboratory 4555 Overlook Ave SW WashingtonDC20375 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Physics Department Occidental College 1600 Campus Road Los AngelesCA90041 United States Space Telescope Science Institute BaltimoreMD21218 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States

It is exceedingly rare to find quiescent low-mass galaxies in the field at low redshift. UGC5205 is an example of such a quenched field dwarf (M* ∼ 3 × 108Mo). Despite a wealth of cold gas (MHI ∼ 3.5 × 108Mo) and ultraviolet emission that indicates significant star formation in the past few hundred Myr, there is no detection of Hα emission - star formation in the last ∼ 10 Myr - across the face of the galaxy. Meanwhile, the near equal-mass companion of UGC5205, PGC027864, is starbursting (EWHα > 1000 Å). In this work, we present new Karl G. Jansky Very Large Array (VLA) 21 cm line observations of UGC5205 showing that the lack of star formation is caused by an absence of H I in the main body of the galaxy. The H I of UGC5205 is highly disturbed;the bulk of the H I resides in several kpc-long tails, while the H I of PGC027864 is dominated by ordered rotation. We model the stellar populations of UGC5205 to show that, as indicated by the UV-Hα emission, the galaxy underwent a coordinated quenching event ∼ 100 − 300 Myr ago. The asymmetry of outcomes for UGC5205 and PGC027864 demonstrate that major mergers can both quench and trigger star formation in dwarfs. However, because the gas remains bound to the system, we suggest that such mergers only temporarily quench star formation. We estimate a total quenched time of ∼ 560 Myr for UGC5205, consistent with established upper limits on the quenched fraction of a few percent for dwarfs in the field. © 2023, CC BY.

关键词： Galaxies

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Dark Matter Search Results from the PandaX-4T Commissioning Run

引用

Physical Review Letters 2021年第26期127卷 261802-261802页

作者： Yue Meng Zhou Wang Yi Tao Abdusalam Abdukerim Zihao Bo Wei Chen Xun Chen Yunhua Chen Chen Cheng Yunshan Cheng Xiangyi Cui Yingjie Fan Deqing Fang Changbo Fu Mengting Fu Lisheng Geng Karl Giboni Linhui Gu Xuyuan Guo Ke Han Changda He Jinrong He Di Huang Yanlin Huang Zhou Huang Ruquan Hou Xiangdong Ji Yonglin Ju Chenxiang Li Mingchuan Li Shu Li Shuaijie Li Qing Lin Jianglai Liu Xiaoying Lu Lingyin Luo Wenbo Ma Yugang Ma Yajun Mao Nasir Shaheed Xuyang Ning Ningchun Qi Zhicheng Qian Xiangxiang Ren Changsong Shang Guofang Shen Lin Si Wenliang Sun Andi Tan Anqing Wang Meng Wang Qiuhong Wang Shaobo Wang Siguang Wang Wei Wang Xiuli Wang Mengmeng Wu Weihao Wu Jingkai Xia Mengjiao Xiao Xiang Xiao Pengwei Xie Binbin Yan Xiyu Yan Jijun Yang Yong Yang Chunxu Yu Jumin Yuan Ying Yuan Dan Zhang Minzhen Zhang Peng Zhang Tao Zhang Li Zhao Qibin Zheng Jifang Zhou Ning Zhou Xiaopeng Zhou Yong Zhou School of Physics and Astronomy Shanghai Jiao Tong University MOE Key Laboratory for Particle Astrophysics and Cosmology Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai 200240 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu 610213 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai 200240 China Yalong River Hydropower Development Company Limited 288 Shuanglin Road Chengdu 610051 China School of Physics Sun Yat-Sen University Guangzhou 510275 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Qingdao 266237 Shandong China Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong University Qingdao 266237 Shandong China School of Physics Nankai University Tianjin 300071 China Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) Institute of Modern Physics Fudan University Shanghai 200433 China School of Physics Peking University Beijing 100871 China School of Physics Beihang University Beijing 100191 China International Research Center for Nuclei and Particles in the Cosmos and Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing 100191 China School of Medical Instrument and Food Engineering University of Shanghai for Science and Technology Shanghai 200093 China Department of Physics University of Maryland College Park Maryland 20742 USA School of Mechanical Engineering Shanghai Jiao Tong University Shanghai 200240 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei 230026 China Department of Modern Physics University of Science and Technology of China Hefei 230026 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai 200240 China

We report the first dark matter search results using the commissioning data from PandaX-4T. Using a time projection chamber with 3.7 tonne of liquid xenon target and an exposure of 0.63 tonne·year, 1058 candidate events are identified within an approximate nuclear recoil energy window between 5 and 100 keV. No significant excess over background is observed. Our data set a stringent limit to the dark matter–nucleon spin-independent interactions, with a lowest excluded cross section (90% C.L.) of 3.8×10−47 cm2 at a dark matter mass of 40 GeV/c2.

关键词： particle dark matter Dark matter detectors

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From Halos to Galaxies. X: Decoding Galaxy SEDs with Physical Priors and Accurate Star Formation History Reconstruction

arXiv

引用

arXiv 2024年

作者： Gao, Zeyu Peng, Yingjie Wang, Kai Ho, Luis C. Renzini, Alvio Gallazzi, Anna R. Mannucci, Filippo Mo, Houjun Jing, Yipeng Yang, Xiaohu Wang, Enci Zhao, Dingyi Dou, Jing Gu, Qiusheng Lyu, Cheqiu Maiolino, Roberto Wang, Bitao Wang, Yu-Chen Xu, Bingxiao Yuan, Feng Zhu, Xingye Department of Astronomy School of Physics Peking University 5 Yiheyuan Road Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom INAF Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy INAF Osservatorio Astrofisico di Arcetri Largo Enrico Fermi 5 FirenzeI-50125 Italy Department of Astronomy University of Massachusetts AmherstMA01003 United States Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Tsung-Dao Lee Institute Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai Jiao Tong University Shanghai200240 China CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China School of Astronomy and Space Science Nanjing University Nanjing210093 China Cavendish Laboratory University of Cambridge 19 J.J. Thomson Avenue CambridgeCB3 0HE United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom School of Physics and Electronics Hunan University Changsha410082 China Center for Astronomy and Astrophysics Department of Physics Fudan University 2005 Songhu Road Shanghai200438 China

The spectral energy distribution (SED) of galaxies is essential for deriving fundamental properties like stellar mass and star formation history (SFH). However, conventional methods, including both parametric and nonparametric approaches, often fail to accurately recover the observed cosmic star formation rate (SFR) density due to oversimplified or unrealistic assumptions about SFH and their inability to account for the complex SFH variations across different galaxy populations. To address this issue, we introduce a novel approach that improves galaxy broadband SED analysis by incorporating physical priors derived from hydrodynamical simulations. Tests using IllustrisTNG simulations demonstrate that our method can reliably determine galaxy physical properties from broadband photometry, including stellar mass within 0.05 dex, current SFR within 0.3 dex, and fractional stellar formation time within0.2 dex, with a negligible fraction of catastrophic failures. When applied to the Sloan Digital Sky Survey (SDSS) main photometric galaxy sample with spectroscopic redshift, our estimates of stellar mass and SFR are consistent with the widely used MPA-JHU and GSWLC catalogs. Notably, using the derived SFHs of individual SDSS galaxies, we estimate the cosmic SFR density and stellar mass density with remarkable consistency to direct observations up to z ∼ 6. This demonstrates a significant advancement in deriving SFHs from SEDs that closely align with observational data. Consequently, our method can reliably recover observed spectral indices such as Dn(4000) and HδA by synthesizing the full spectra of galaxies using the estimated SFHs and metal enrichment histories, relying solely Copyright © 2024, The Authors. All rights reserved.

关键词： cosmology

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