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Determination of responses of liquid xenon to low energy electron and nuclear recoils using a PandaX-Ⅱ detector

Chinese physics C 2021年第7期45卷 273-282页

作者： Binbin Yan Abdusalam Abdukerim Wei Chen Xun Chen Yunhua Chen Chen Cheng Xiangyi Cui Yingjie Fan Deqing Fang Changbo Fu Mengting Fu Lisheng Geng Karl Giboni Linhui Gu Xuyuan Guo Ke Han Changda He Di Huang Peiyao Huang Yan Huang Yanlin Huang Zhou Huang Xiangdong Ji Yonglin Ju Shuaijie Li Jianglai Liu Zhuoqun Lei Wenbo Ma Yugang Ma Yajun Mao Yue Meng Kaixiang Ni Jinhua Ning Xuyang Ning Xiangxiang Ren Changsong Shang Lin Si Guofang Shen 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 Pengwei Xie Rui Yan Jijun Yang Yong Yang Chunxu Yu Jumin Yuan Ying Yuan Jianfeng Yue Xinning Zeng Dan Zhang Tao Zhang Li Zhao Qibin Zheng Jifang Zhou Ning Zhou Xiaopeng Zhou School of Physics and Astronomy Shanghai Jiao Tong UniversityMOE Key Laboratory for Particle Astrophysics and CosmologyShanghai Key Laboratory for Particle Physics and CosmologyShanghai 200240China Shanghai Institute of Applied Physics Chinese Academy of SciencesShanghai 201800China Key Laboratory of Nuclear Physics and Ion-beam Application(MOE) Institute of Modern PhysicsFudan UniversityShanghai 200433China Shanghai Jiao Tong University Sichuan Research Institute Chengdu 610213China Yalong River Hydropower Development Company Ltd.288 Shuanglin RoadChengdu 610051China School of Physics Sun Yat-Sen UniversityGuangzhou 510275China Tsung-Dao Lee Institute Shanghai 200240China School of Physics Nankai UniversityTianjin 300071China School of Physics Peking UniversityBeijing 100871China School of Physics Beihang UniversityBeijing 100191China International Research Center for Nuclei and Particles in the Cosmos&Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang UniversityBeijing 100191China School of Medical Instrument and Food Engineering University of Shanghai for Science and TechnologyShanghai 200093China Department of Physics University of MarylandCollege ParkMaryland 20742USA School of Mechanical Engineering Shanghai Jiao Tong UniversityShanghai 200240China School of Physics and Key Laboratory of Particle Physics and Particle Irradiation(MOE) Shandong UniversityJinan 250100China Shanghai Advanced Research Institute Chinese Academy of SciencesShanghai 201210China Center for High Energy Physics Peking UniversityBeijing 100871China

We present a systematic determination of the responses of PandaX-Ⅱ,a dual phase xenon time projection chamber detector,to low energy *** electron recoil(ER) and nuclear recoil(NR) responses are calibrated,respectively,with injected tritiated methane or 220Rn source,and with 241Am-Be neutron source,in an energy range from 1-25 keV(ER) and 4-80 keV(NR),under the two drift fields,400 and 317 V/*** empirical model is used to fit the light yield and charge yield for both types of *** best fit models can describe the calibration data *** systematic uncertainties of the fitted models are obtained via statistical comparison to the data.

关键词： dark matter liquid xenon time projection chamber calibration electron recoil nucleon recoil NEST2.0

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Wide Binary Evaporation by Dark Solitons: Implications from the GAIA Catalog

arXiv

引用

arXiv 2024年

作者： Qiu, Qiming Gao, Yu Tian, Haijun Wang, Kechen Wang, Zihang Yang, Xiangming Beijing100190 China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China School of Science Hangzhou Dianzi University Hangzhou310018 China Department of Physics School of Physics and Mechanics Wuhan University of Technology Hubei Wuhan430070 China Zhejiang Branch of National Astronomical Data Center Hangzhou310018 China

An analytic calculation is given for binary star evaporation under the tidal perturbation from randomly distributed, spatially extended dark objects. In particular, the Milky Way’s wide binary star population is susceptible to such disruption from dark matter solitons of comparable and larger sizes. We identify high-probability ‘halo-like’ wide binaries in GAIA EDR3 with separations larger than 0.1 parsec. Survival of the farthest-separated candidates will provide a novel gravitational probe to dark matter in the form of solitons. In the case of dilute axion-like boson stars, the observational sensitivity extends into the axion mass range ma ∼ 10−17 − 10−15 eV. Copyright © 2024, The Authors. All rights reserved.

关键词： Solitons

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Constraining primordial black holes as dark matter using AMS-02 data

arXiv

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arXiv 2024年

作者： Su, Bing-Yu Pan, Xu Wang, Guan-Sen Zu, Lei Yang, Yupeng Feng, Lei Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China School of Physics and Physical Engineering Qufu Normal University Shandong Qufu273165 China Joint Center for Particle Nuclear Physics and Cosmology Nanjing University-Purple Mountain Observatory Nanjing210093 China

Primordial black holes (PBHs) are the plausible candidates for the cosmological dark matter. Theoretically, PBHs with masses MPBH in the range of 4 × 1014 ∼ 1017 g can emit sub-GeV electrons and positrons through Hawking radiation. Some of these particles could undergo diffusive reacceleration during propagation in the Milky Way, potentially reaching energies up to the GeV level observed by AMS-02. In this work, we utilize AMS-02 data to constrain the PBH abundance fPBH by employing the reacceleration mechanism. Under the assumption of a monochromatic PBH mass distribution, our findings reveal that the limit is stricter than that derived from Voyager 1 data. This difference is particularly pronounced when MPBH 1015 g, exceeding an order of magnitude. The constraints are even more robust in a more realistic scenario involving a log-normal mass distribution of PBHs. Moreover, we explore the impact of varying propagation parameters and solar modulation potential within reasonable ranges, and find that such variations have minimal effects on the final results. Copyright © 2024, The Authors. All rights reserved.

关键词： Germanium alloys

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Equivariant geometric convolutions for emulation of dynamical systems

arXiv

引用

arXiv 2023年

作者： Gregory, Wilson G. Hogg, David W. Blum-Smith, Ben Arias, Maria Teresa Wong, Kaze W.K. Villar, Soledad Department of Applied Mathematics and Statistics Johns Hopkins University BaltimoreMD United States Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY United States Max-Planck-Institut für Astronomie Heidelberg Germany Center for Computational Astrophysics Flatiron Institute New YorkNY United States Department of Mathematics Universidad Autónoma de Madrid Madrid Spain Mathematical Institute for Data Science Johns Hopkins University BaltimoreMD United States

Machine learning methods are increasingly being employed as surrogate models in place of computationally expensive and slow numerical integrators for a bevy of applications in the natural sciences. However, while the laws of physics are relationships between scalars, vectors, and tensors that hold regardless of the frame of reference or chosen coordinate system, surrogate machine learning models are not coordinate-free by default. We enforce coordinate freedom by using geometric convolutions in three model architectures: a ResNet, a Dilated ResNet, and a UNet. In numerical experiments emulating 2D compressible Navier-Stokes, we see better accuracy and improved stability compared to baseline surrogate models in almost all cases. The ease of enforcing coordinate freedom without making major changes to the model architecture provides an exciting recipe for any CNN-based method applied to an appropriate class of problems. © 2023, CC BY.

关键词： Convolution

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Induced gravitational waves with kination era for recent pulsar timing array signals

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Physical Review D 2023年第12期108卷 123538-123538页

作者： Keisuke Harigaya Keisuke Inomata Takahiro Terada Department of Physics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics and Enrico Fermi Institute University of Chicago Chicago Illinois 60637 USA Kavli Institute for the Physics and Mathematics of the Universe (WPI) The University of Tokyo Institutes for Advanced Study 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

The evidence of the stochastic gravitational-wave background around the nanohertz frequency range was recently found by worldwide pulsar timing array (PTA) collaborations. One of the cosmological explanations is the gravitational waves induced by enhanced curvature perturbations, but the issue of primordial black hole (PBH) overproduction in this scenario was pointed out in the literature. Motivated by this issue and the ΩGW∼f2 scaling suggested by the data, we study the gravitational waves induced in a cosmological epoch dominated by a stiff fluid (w=1) and find that they can safely explain the PTA data well without PBH overproduction.

关键词： cosmology Evolution of the Universe Gravitational wave sources Gravitational waves

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Gravitational wave production from axion rotations right after a transition to kination

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Physical Review D 2023年第8期108卷 L081303-L081303页

Rotations of axion fields in the early Universe can produce dark matter and the matter-antimatter asymmetry of the Universe. We point out that the rotation can generate an observable amount of a stochastic gravitational wave (GW) background. It can be doubly enhanced in a class of models in which the equation of state of the rotations rapidly changes from a nonrelativistic matterlike one to a kinationlike one by (1) the so-called poltergeist mechanism and (2) slower redshift of GWs compared to the axion-kination fluid. In supersymmetric UV completion, future GW observations can probe the supersymmetry-breaking scale up to 107 GeV even if the axion does not directly couple to the Standard Model fields.

关键词： cosmology Gravitational waves particle astrophysics Axion-like particles Axions Supersymmetry

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Indirect detection of long-lived particles in a rich dark sector with a dark vector portal

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Physical Review D 2023年第11期108卷 115026-115026页

作者： Krzysztof Jodłowski Leszek Roszkowski Sebastian Trojanowski Particle Theory and Cosmology Group Center for Theoretical Physics of the Universe Institute for Basic Science (IBS) Daejeon 34126 Korea and National Centre for Nuclear Research Pasteura 7 02-093 Warsaw Poland Astrocent Nicolaus Copernicus Astronomical Center Polish Academy of Sciences ul. Bartycka 18 00-716 Warsaw Poland and National Centre for Nuclear Research Pasteura 7 02-093 Warsaw Poland

Simplified models of light new physics provide a convenient benchmark for experimental searches for new physics signatures, including dark matter (DM). However, additional detection modes can arise in less simplified and more realistic scenarios where new degrees of freedom are invoked. In this study, we introduce a nonminimal model based on a popular dark photon portal to DM where the mediator mass is obtained by interactions with the dark Higgs boson which acts as a long-lived particle. We further add to this scenario a new heavy DM species secluded from the Standard Model. In this model, which involves light and heavy particles in the dark sector, we find some new interesting phenomenological features that lead to complementary probes in intensity frontier searches for light long-lived particles, indirect detection searches for dark matter, and cosmic microwave background surveys. We also find possible nonlocal effects in the DM indirect detection searches that could significantly affect the usual detection strategies.

关键词： Dark matter particle dark matter

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Highlight of LHAASO science results on PeVatrons 38

Highlight of LHAASO science results on PeVatrons

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Wu, Sha Chen, Songzhan 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. Sun, Q.N. Sun, X.N. Sun, Z.B. Tam, P.H.T. Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Key Laboratory of Particle Astrophysics Experimental Physics Division Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu 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 Yat-sen University Guangdong Guangzhou510275 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-sen University Zhuhai519000 China School of Physics and Astronomy Yunnan University Yunnan

The observation of ultra-high energy (UHE, E>100 TeV) gamma-ray sources plays a crucial role in identifying Galactic PeV accelerators, also known as PeVatrons. The Large High Altitude Air Shower Observatory (LHAASO) is a large hybrid extensive air shower array, constructed at Haizi Mountain, 4410 m a.s.l., in China. With its wide field of view and high sensitivity, LHAASO is an ideal instrument for the detection and study of PeVatrons within our Galaxy. Since July 2021, the whole LHAASO detector array has been completed and operated in good states. Through an all-sky survey, we have observed ultra-high energy gamma-ray emissions in 43 regions associated with pulsars, supernova remnants (SNR), young star clusters, and other celestial objects. In this proceeding, we will present the results obtained from representative gamma-ray sources and discuss our observations of diffuse gamma-ray emissions along the Galactic plane. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Supernovae

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One-loop tensor power spectrum from an excited scalar field during inflation

引用

Physical Review D 2023年第4期108卷 043542-043542页

作者： Atsuhisa Ota Misao Sasaki Yi Wang HKUST Jockey Club Institute for Advanced Study The Hong Kong University of Science and Technology Clear Water Bay Hong Kong People’s Republic of China Kavli Institute for the Physics and Mathematics of the Universe (WPI) University of Tokyo Chiba 277-8583 Japan Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kyoto 606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei 10617 Department of Physics The Hong Kong University of Science and Technology Clear Water Bay Hong Kong People’s Republic of China

We present a consistent one-loop calculation for the inflationary tensor power spectrum in the presence of an excited spectator scalar field using the in-in formalism. We find that the superhorizon primordial power spectrum of the tensor mode can be scale-invariantly enhanced or reduced by the loop effects of a subhorizon scalar field. Our calculation also includes the scalar-induced gravitational wave spectrum classically computed in the previous literature, which is significant only near the scales where the scalar field is amplified. The superhorizon enhancement is a higher-order effect of the interaction Hamiltonian, which can be understood as a Bogoliubov transformation introduced by nonlinear interactions. On the other hand, the scale-invariant reduction of the tensor power spectrum may occur due to the fourth-order scalar-scalar-tensor-tensor coupling. This phenomenon can be understood as the evolution of an anisotropic Bianchi type-I background in the separate universe approach. Our result suggests that large-scale measurements may indirectly test the dramatic effects of small-scale cosmological perturbations through loop corrections. This possibility opens a new ground in probing the small-scale physics of the primordial Universe through gravitational wave detectors of cosmological scales.

关键词： Cosmic microwave background Gravitational waves Inflation

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Possibilities for methanogenic and acetogenic life in molecular cloud

arXiv

引用

arXiv 2023年

作者： Feng, Lei Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China Joint Center for Particle Nuclear Physics and Cosmology Nanjing University Purple Mountain Observatory Nanjing210093 China

According to panspermia, life on Earth may have originated from life forms transported through space from elsewhere. These life forms could have passed through molecular clouds, where the process of methanogenesis could have provided enough energy to sustain living organisms. In this study, we have calculated the Gibbs free energy released from synthesizing hydrocarbons for methanogenic (acetogenic) life in a molecular cloud, with methane (acetic acid) as the final metabolic product. Our calculations demonstrate that the chemical reactions during methanogenesis can release enough free energy to support living organisms. The methanogenic life may have served as the predecessor of life on Earth, and there is some preliminary evidence from various molecular biology studies to support this idea. Furthermore, we propose a potential distinguishing signal to test our model. Copyright © 2023, The Authors. All rights reserved.

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