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Statistical constraints on climate model parameters using a scalable cloud-based inference framework

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arXiv 2023年

作者： Carzon, James Abreu, Bruno Regayre, Leighton Carslaw, Kenneth Deaconu, Lucia Stier, Philip Gordon, Hamish Kuusela, Mikael Department of Statistics and Data Science Carnegie Mellon University PittsburghPA United States National Center for Supercomputing Applications University of Illinois Urbana-Champaign Urbana-ChampaignIL United States Institute for Climate and Atmospheric Science School of Earth and Environment University of Leeds Leeds United Kingdom Met Office Hadley Centre Exeter United Kingdom Atmospheric Oceanic and Planetary Physics Department University of Oxford Oxford United Kingdom Faculty of Environmental Science and Engineering Babes-Bolyai University Cluj Romania Department of Chemical Engineering Carnegie Mellon University PittsburghPA United States Center for Atmospheric Particle Studies Carnegie Mellon University PittsburghPA United States NSF AI Planning Institute for Data-Driven Discovery in Physics Carnegie Mellon University PittsburghPA United States

Atmospheric aerosols influence the Earth’s climate, primarily by affecting cloud formation and scattering visible radiation. However, aerosol-related physical processes in climate simulations are highly uncertain. Constraining these processes could help improve model-based climate predictions. We propose a scalable statistical framework for constraining parameters in expensive climate models by comparing model outputs with observations. Using the *** Suite, a cloud computing platform, we use a perturbed parameter ensemble of the UKESM1 climate model to efficiently train a surrogate model. A method for estimating a data-driven model discrepancy term is described. The strict bounds method is applied to quantify parametric uncertainty in a principled way. We demonstrate the scalability of this framework with two weeks’ worth of simulated aerosol optical depth data over the South Atlantic and Central African region, written from the model every three hours and matched in time to twice-daily MODIS satellite observations. When constraining the model using real satellite observations, we establish constraints on combinations of two model parameters using much higher time-resolution outputs from the climate model than previous studies. This result suggests that, within the limits imposed by an imperfect climate model, potentially very powerful constraints may be achieved when our framework is scaled to the analysis of more observations and for longer time periods. © 2023, CC BY.

关键词： Climate models

The Multiband Imaging Survey for High-Alpha PlanetS (MISHAPS) I: Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae

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arXiv 2024年

作者： Crisp, Alison L. Klüter, Jonas Newman, Marz L. Penny, Matthew T. Beatty, Thomas G. Cleeves, L. Ilsedore Collins, Karen A. Johnson, Jennifer A. Johnson, Marshall C. Lund, Michael B. Martínez-Vázquez, Clara E. Ness, Melissa K. Rodriguez, Joseph E. Siverd, Robert Stevens, Daniel J. Villanueva, Steven Ziegler, Carl Department of Physics & Astronomy Louisiana State University Baton RougeLA70803 United States Department of Astronomy The Ohio State University ColumbusOH43210 United States Center for Computation & Technology Louisiana State University Baton RougeLA70803 United States Department of Astronomy University of Wisconsin – Madison MadisonWI53706 United States Department of Astronomy University of Virginia CharlottesvilleVA22904 United States Department of Chemistry University of Virginia CharlottesvilleVA22904 United States Harvard-Smithsonian Center for Astrophysics CambridgeMA02138 United States Center for Cosmology & Astro Particle Physics The Ohio State University ColumbusOH43210 United States NASA Exoplanet Science Institute California Institute of Technology PasadenaCA91125 United States Gemini North Observatory NOIRLab HiloHI96720 United States Department of Astronomy Columbia University New YorkNY10027 United States Simons Center for Computational Astrophysics Flatiron Institute New YorkNY10004 United States Center for Data Intensive and Time Domain Astronomy Department of Physics & Astronomy Michigan State University East LansingMI48824 United States Institute for Astronomy University of Hawai’i at Mānoa HonoluluHI96822 United States Department of Physics & Astronomy University of Minnesota – Duluth DuluthMN55812 United States Exoplanets & Stellar Astrophysics Laboratory NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Physics Engineering & Astronomy Stephen F. Austin State University NacogdochesTX75962 United States

The first generation of transiting planet searches in globular clusters yielded no detections, and in hindsight, only placed occurrence rate limits slightly higher than the measured occurrence rate in the higher-metallicity Galactic thick disk. To improve these limits, we present the first results of a new wide field search for transiting hot Jupiters in the globular cluster 47 Tucanae. We have observed 47 Tuc as part of the Multiband Imaging Survey for High-Alpha Planets (MISHAPS). Using 24 partial and full nights of observations taken with the Dark Energy Camera on the 4-m Blanco telescope at CTIO, we perform a search on 19,930 stars in the outer regions of the cluster. Though we find no clear planet detections, by combining our result with the upper limit enabled by Gilliland et al.’s (2000) Hubble search for planets around an independent sample of 34,091 stars in the inner cluster, we place the strongest limit to date on hot Jupiters with periods of 0.8 ≤ P ≤ 8.3 days and 0.5 RJup ≤ RP ≤ 2.0 RJup of fHJ © 2024, CC BY.

关键词： Stars

The YAG Lidar System Applied in LHAASO 37

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The YAG Lidar System Applied in LHAASO

37th International Cosmic Ray Conference, ICRC 2021

作者： Sun, Q.N. Geng, L.S. Li, X. Chen, L. Liu, H. Wang, Y. Zhu, F.R. Zhang, Y. Cao, Zhen Aharonian, F. An, Q. Axikegu Bai, L.X. Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Cai, H. Cai, J.T. Cao, Zhe Chang, J. Chang, J.F. Chen, B.M. Chen, E.S. Chen, J. Chen, Liang Chen, Liang Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, X.L. Chen, Y. Cheng, N. Cheng, Y.D. Cui, S.W. Cui, X.H. Cui, Y.D. D’Ettorre Piazzoli, B. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu della Volpe, D. Dong, X.J. Duan, K.K. Fan, J.H. Fan, Y.Z. Fan, Z.X. Fang, J. Fang, K. Feng, C.F. Feng, L. Feng, S.H. Feng, Y.L. Gao, B. Gao, C.D. Gao, L.Q. Gao, Q. Gao, W. Ge, M.M. Geng, L.S. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, J.G. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. He, H.H. He, H.N. He, J.C. He, S.L. He, X.B. He, Y. Heller, M. Hor, Y.K. Hou, C. Hu, H.B. Hu, S. Hu, S.C. Hu, X.J. Huang, D.H. Huang, Q.L. Huang, W.H. Huang, X.T. Huang, X.Y. Huang, Z.C. Ji, F. Ji, X.L. Jia, H.Y. Jiang, K. Jiang, Z.J. Jin, C. Ke, T. Kuleshov, D. Levochkin, K. Li, B.B. Li, Cheng Li, Cong Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, K. Li, W.L. Li, X.R. Li, Xin Li, Xin Li, Y. 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.S. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Liu, Z.X. Long, W.J. Lu, R. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Masood, A. Min, Z. Mitthumsiri, W. Montaruli, T. Nan, Y.C. Pang, B.Y. Pattarakijwanich, P. Pei, Z.Y. Qi, M.Y. Qi, Y.Q. Qiao, B.Q. Qin, J.J. Ruffolo, D. Rulev, V. Sáiz, A. Shao, L. Shchegolev, O. Sheng, X.D. Shi, J.Y. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Sun, Q.N. Sun, X.N. Sun, Z.B. Tam, P.H.T. School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Sichuan Chengdu610031 China Key Laboratory of Particle Astrophyics Experimental Physics Division Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu China Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin02 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 College of Physics Sichuan University Sichuan Chengdu610065 China School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210023 China Center for Astrophysics Guangzhou University Guangdong Guangzhou510006 China School of Physics and Technology Wuhan University Hubei Wuhan430072 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Hebei Normal University Hebei Shijiazhuang050024 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Ministry of Education Tibet Lhasa850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Sun Yat-sen University Guangdong Zhuhai519000 China Dipartimento di Fisica dell’Università di Napoli `‘Federico II" Complesso Universitario di Monte Sant’Angelo

The atmospheric quality plays an important role in the air shower observation by the Wide Field-of-view Cherenkov Telescope Array (WFCTA) of LHAASO. A YAG imaging lidar system was developed to continuously monitor the calorimetric information. The accuracy of atmospheric monitoring is dependent on the pulse energy, the YAG laser’s beam parameters and the angular repeatability of a High-precision 3D lifting Rotating Platform (HiRoP). Therefore, we designed an optical system for this lidar with a beam splitter to divide the laser beam into a reference beam and a calibrating beam with a certain ratio and coupled the beam paths with the movement of HiRoP. Thus, every pulse energy of the calibrating beam, which has the same energy fluctuation with respect to the reference beam recorded by a power meter, could be calculated by the ratio of the two beams. Great cares were also taken to characterize the beam size, polarization and divergence of the laser. Meanwhile, a high-precision home-made thermotank was designed to control the temperature and humidity to improve the performance and stability of our laser system, which resulting in a thermal fluctuation less than 2 ◦C inside the container in the winter at an altitude of 4410 m. As a result, the pulse energy fluctuation of the laser beam for calibration was improved from 5 % to less than 2 %. As a result, we have successfully attained distinguishable full-WFCTA-view scanning Laser images in different air conditions, which could be used for the atmospheric quality analysis in further. © Copyright owned by the author(s).

关键词： Yttrium aluminum garnet

Effects of atmospheric transparency on Telescope Array air shower analysis 38

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Effects of atmospheric transparency on Telescope Array air s...

38th International Cosmic Ray Conference, ICRC 2023

作者： Mizuno, K. Tomida, T. Yamazaki, K. Abbasi, R.U. Abe, Y. Abu-Zayyad, T. Allen, M. Arai, Y. Arimura, R. Barcikowski, E. Belz, J.W. Bergman, D.R. Blake, S.A. Buckland, I. Cheon, B.G. Chikawa, M. Fedynitch, A. Fujii, T. Fujisue, K. Fujita, K. Fujiwara, R. Fukushima, M. Furlich, G. Gerber, Z. Globus, N. Hanlon, W. Hayashida, N. He, H. Hibi, R. Hibino, K. Higuchi, R. Honda, K. Ikeda, D. Inoue, N. Ishii, T. Ito, H. Ivanov, D. Iwasaki, A. Jeong, H.M. Jeong, S. Jui, C.C.H. Kadota, K. Kakimoto, F. Kalashev, O. Kasahara, K. Kasami, S. Kawakami, S. Kawata, K. Kharuk, I. Kido, E. Kim, H.B. Kim, J.H. Kim, J.H. Kim, S.W. Kimura, Y. Komae, I. Komori, K. Kusumori, Y. Kuznetsov, M. Kwon, Y.J. Lee, K.H. Lee, M.J. Lubsandorzhiev, B. Lundquist, J.P. Matsuyama, T. Matthews, J.A. Matthews, J.N. Mayta, R. Miyashita, K. Mizuno, K. Mori, M. Murakami, M. Myers, I. Nagataki, S. Nakai, K. Nakamura, T. Nishio, E. Nonaka, T. Ogio, S. Ohoka, H. Okazaki, N. Oku, Y. Okuda, T. Omura, Y. Onishi, M. Ono, M. Oshima, A. Oshima, H. Ozawa, S. Park, I.H. Park, K.Y. Potts, M. Pshirkov, M.S. Remington, J. Rodriguez, D.C. Rott, C. Rubtsov, G.I. Ryu, D. Sagawa, H. Saito, R. Sakaki, N. Sako, T. Sakurai, N. Sato, D. Sato, K. Sato, S. Sekino, K. Shah, P.D. Shibata, N. Shibata, T. Shikita, J. Shimodaira, H. Shin, B.K. Shin, H.S. Shinto, D. Smith, J.D. Sokolsky, P. Stokes, B.T. Stroman, T.A. Takagi, Y. Takahashi, K. Takamura, M. Takeda, M. Takeishi, R. Taketa, A. Takita, M. Tameda, Y. Tanaka, K. Tanaka, M. Thomas, S.B. Thomson, G.B. Tinyakov, P. Tkachev, I. Tokuno, H. Tomida, T. Troitsky, S. Tsuda, R. Tsunesada, Y. Udo, S. Urban, F. Vaiman, I.A. Warren, D. Wong, T. Yamazaki, K. Yashiro, K. Yoshida, F. Zhezher, Y. Zundel, Z. Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano Japan Mathematical and Physical Sciences Science and Engineering Chubu University Aichi Kasugai Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano380-8554 Japan High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT84112-0830 United States Graduate School of Science Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Department of Physics The Research Institute of Natural Science Hanyang University Seongdong-gu Seoul426-791 Korea Republic of Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Institute of Physics Academia Sinica Taipei City115201 Taiwan Nambu Yoichiro Institute of Theoretical and Experimental Physics Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Astrophysical Big Bang Laboratory RIKEN Wako Saitama351-0198 Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama221-8686 Japan Interdisciplinary Graduate School of Medicine and Engineering University of Yamanashi Kofu Yamanashi400-8511 Japan The Graduate School of Science and Engineering Saitama University Saitama Saitama338-8570 Japan Department of Physics SungKyunKwan University Jang-an-gu Suwon16419 Korea Republic of Department of Physics Tokyo City University Setagaya-ku Tokyo158-8557 Japan Institute for Nuclear Research The Russian Academy of Sciences Moscow117312 Russia Faculty of Systems Engineering and Science Shibaura Institute of Technology Minato-ku Tokyo337-8570 Japan Graduate School of Engineering Osaka Electro-Communication University Neyagawa-shi Osaka572-8530 Japan Service de Physique Théorique Université Libre de Bruxelles Brussels Belgium Department of Physics

The Telescope Array (TA) experiment continues to observe Ultra High Energy Cosmic Rays (UHECRs) both with its original TA detectors as well as with the new TAx4 expansion detectors. These observations employ Fluorescence Detectors (FDs) to capture the air shower induced by the primary UHECRs. The FD observes fluorescence light emitted from atmospheric nitrogen molecules excited by air shower particles. Observation of the FD extends over tens of kilometers, and the fluorescence light is attenuated by scattering from atmospheric molecules and aerosols during the propagation process. Seasonal dependence was found when evaluating the attenuation of fluorescence by aerosols. We will report on the effects of this seasonal dependence on TA air shower analysis. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Fluorescence

Observation of Seven Astrophysical Tau Neutrino Candidates with IceCube

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Physical Review Letters 2024年第15期132卷 151001-151001页

作者： R. Abbasi M. Ackermann J. Adams S. K. Agarwalla J. A. Aguilar M. Ahlers J. M. Alameddine N. M. Amin K. Andeen G. Anton C. Argüelles Y. Ashida S. Athanasiadou S. N. Axani X. Bai V. A. Balagopal M. Baricevic S. W. Barwick V. Basu R. Bay J. J. Beatty J. Becker Tjus J. Beise C. Bellenghi C. Benning S. BenZvi D. Berley E. Bernardini D. Z. Besson E. Blaufuss S. Blot F. Bontempo J. Y. Book C. Boscolo Meneguolo S. Böser O. Botner J. Böttcher E. Bourbeau J. Braun B. Brinson J. Brostean-Kaiser R. T. Burley R. S. Busse D. Butterfield M. A. Campana K. Carloni E. G. Carnie-Bronca S. Chattopadhyay N. Chau C. Chen Z. Chen D. Chirkin S. Choi B. A. Clark L. Classen A. Coleman G. H. Collin A. Connolly J. M. Conrad P. Coppin P. Correa D. F. Cowen P. Dave C. De Clercq J. J. DeLaunay D. Delgado S. Deng K. Deoskar A. Desai P. Desiati K. D. de Vries G. de Wasseige T. DeYoung A. Diaz J. C. Díaz-Vélez M. Dittmer A. Domi H. Dujmovic M. A. DuVernois T. Ehrhardt P. Eller E. Ellinger S. El Mentawi D. Elsässer R. Engel H. Erpenbeck J. Evans P. A. Evenson K. L. Fan K. Fang K. Farrag A. R. Fazely N. Feigl S. Fiedlschuster A. T. Fienberg C. Finley L. Fischer D. Fox A. Franckowiak A. Fritz P. Fürst J. Gallagher E. Ganster A. Garcia L. Gerhardt A. Ghadimi C. Glaser T. Glauch T. Glüsenkamp N. Goehlke J. G. Gonzalez S. Goswami D. Grant S. J. Gray O. Gries S. Griffin S. Griswold K. M. Groth C. Günther P. Gutjahr C. Haack A. Hallgren R. Halliday L. Halve F. Halzen H. Hamdaoui M. Ha Minh K. Hanson J. Hardin A. A. Harnisch P. Hatch A. Haungs K. Helbing J. Hellrung F. Henningsen L. Heuermann N. Heyer S. Hickford A. Hidvegi C. Hill G. C. Hill K. D. Hoffman S. Hori K. Hoshina W. Hou T. Huber K. Hultqvist M. Hünnefeld R. Hussain K. Hymon S. In A. Ishihara M. Jacquart O. Janik M. Jansson G. S. Japaridze M. Jeong M. Jin B. J. P. Jones D. Kang W. Kang X. Kang A. Kappes D. Kappesser L. Kardum T. Karg M. Karl A. Karle U. Katz M. Kauer J. L. Kelley A. Khatee Zathul A. Kheirandish J. Kiryluk S. R. Klein A. Kochocki R. Koirala H. Kolanoski T. Kontrimas L. Köpke C. Department of Physics Loyola University Chicago Chicago Illinois 60660 USA Deutsches Elektronen-Synchrotron DESY Platanenallee 6 15738 Zeuthen Germany Department of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Department of Physics and Wisconsin IceCube Particle Astrophysics Center University of Wisconsin–Madison Madison Wisconsin 53706 USA Université Libre de Bruxelles Science Faculty CP230 B-1050 Brussels Belgium Niels Bohr Institute University of Copenhagen DK-2100 Copenhagen Denmark Department of Physics TU Dortmund University D-44221 Dortmund Germany Bartol Research Institute and Department of Physics and Astronomy University of Delaware Newark Delaware 19716 USA Department of Physics Marquette University Milwaukee Wisconsin 53201 USA Erlangen Centre for Astroparticle Physics Friedrich-Alexander-Universität Erlangen-Nürnberg D-91058 Erlangen Germany Department of Physics and Laboratory for Particle Physics and Cosmology Harvard University Cambridge Massachusetts 02138 USA Department of Physics and Astronomy University of Utah Salt Lake City Utah 84112 USA Physics Department South Dakota School of Mines and Technology Rapid City South Dakota 57701 USA Department of Physics and Astronomy University of California Irvine California 92697 USA Department of Physics University of California Berkeley California 94720 USA Department of Astronomy Ohio State University Columbus Ohio 43210 USA Department of Physics and Center for Cosmology and Astro-Particle Physics Ohio State University Columbus Ohio 43210 USA Fakultät für Physik & Astronomie Ruhr-Universität Bochum D-44780 Bochum Germany Department of Physics and Astronomy Uppsala University Box 516 S-75120 Uppsala Sweden Physik-department Technische Universität München D-85748 Garching Germany III. Physikalisches Institut RWTH Aachen University D-52056 Aachen Germany Department of Physics and Astronomy University of Rochester Rochester New York 1

We report on a measurement of astrophysical tau neutrinos with 9.7 yr of IceCube data. Using convolutional neural networks trained on images derived from simulated events, seven candidate ντ events were found with visible energies ranging from roughly 20 TeV to 1 PeV and a median expected parent ντ energy of about 200 TeV. Considering backgrounds from astrophysical and atmospheric neutrinos, and muons from π±/K± decays in atmospheric air showers, we obtain a total estimated background of about 0.5 events, dominated by non-ντ astrophysical neutrinos. Thus, we rule out the absence of astrophysical ντ at the 5σ level. The measured astrophysical ντ flux is consistent with expectations based on previously published IceCube astrophysical neutrino flux measurements and neutrino oscillations.

关键词： Cosmic ray acceleration Extrasolar neutrino astronomy particle interactions particle mixing & oscillations Cherenkov detectors Machine learning Neutrino detection Telescopes

Search for light dark matter from atmosphere in PandaX-4T

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arXiv 2023年

作者： Ning, Xuyang Abdukerim, Abdusalam Bo, Zihao Chen, Wei Chen, Xun 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, Junting Huang, Zhou Hou, Ruquan Hou, Yu Ji, Xiangdong Ju, Yonglin Li, Chenxiang Li, Jiafu Li, Mingchuan Li, Shuaijie Li, Tao Lin, Qing Liu, Jianglai Lu, Congcong Lu, Xiaoying Luo, Lingyin Luo, Yunyang Ma, Wenbo Ma, Yugang Mao, Yajun Meng, Yue Qi, Ningchun Qian, Zhicheng Ren, Xiangxiang Shaheed, Nasir Shang, Xiaofeng Shao, Xiyuan 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, Mengmeng Wu, Weihao Xia, Jingkai Xiao, Mengjiao Xiao, Xiang Xie, Pengwei Yan, Binbin Yan, Xiyu Yang, Jijun Yang, Yong Yao, Yukun Yu, Chunxu Yuan, Ying Yuan, Zhe Zeng, Xinning Zhang, Dan Zhang, Minzhen Zhang, Peng Zhang, Shibo Zhang, Shu Zhang, Tao Zhang, Wei Zhang, Yang Zhang, Yingxin Zhang, Yuanyuan Zhao, Li Zheng, Qibin Zhou, Jifang Zhou, Ning Zhou, Xiaopeng Zhou, Yong Zhou, Yubo Su, Liangliang Wu, Lei Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu610213 China School of Physics Sun Yat-Sen University Guangzhou510275 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai519082 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai200240 China Department of Physics Yantai University Yantai264005 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 Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu610051 China School of Medical Instrument and Food Engineering University of Shanghai for Science and Technology Shanghai200093 China School of Mechanical Engineering Shanghai Jiao Tong University Shanghai200240 China Department of Physics University of Maryland College ParkMD20742 United States 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 Ministry of Education Shandong University Shandong Qingdao266237 China School of Physics Nankai University Tianjin300071 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai200240 China School of Physics and Astronomy Sun Y

We report a search for light dark matter produced through the cascading decay of η mesons, which are created as a result of inelastic collisions between cosmic rays and Earth's atmosphere. We introduces a new and general framework, publicly accessible, designed to address boosted dark matter specifically, with which a full and dedicated simulation including both elastic and quasi-elastic processes of Earth attenuation effect on the dark matter particles arriving at the detector is performed. In the PandaX-4T commissioning data of 0.63 tonne·year exposure, no significant excess over background is observed. The first constraints on the interaction between light dark matter generated in the atmosphere and nucleus through a light scalar mediator are obtained. The lowest excluded cross-section is set at 5.9 × 10−37cm2 for dark matter mass of 0.1 MeV/c2 and mediator mass of 300 MeV/c2. The lowest upper limit of η to dark matter decay branching ratio is 1.6 × 10−7 Copyright © 2023, The Authors. All rights reserved.

关键词： Earth atmosphere

Beating the Lyth Bound by Parametric Resonance during Inflation

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Physical Review Letters 2021年第25期127卷 251301-251301页

作者： Yi-Fu Cai Jie Jiang Misao Sasaki Valeri Vardanyan Zihan Zhou Department of Astronomy School of Physical Sciences University of Science and Technology of China Hefei Anhui 230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei Anhui 230026 China CAS Key Laboratory for Researches in Galaxies and Cosmology University of Science and Technology of China Hefei Anhui 230026 China Kavli Institute for the Physics and Mathematics of the Universe (WPI) UTIAS The University of Tokyo Chiba 277-8583 Japan Center for Gravitational Physics Yukawa Institute for Theoretical Physics Kyoto University Kyoto 606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei 10617 Taiwan

We propose a novel mechanism for enhancing primordial gravitational waves without significantly affecting the curvature perturbations produced during inflation. This is achieved due to nonlinear sourcing of resonantly amplified scalar field fluctuations. Our result is an explicit scale-dependent counterexample of the famous Lyth bound, which opens up a promising perspective of producing detectable inflationary tensor modes with low-scale inflation and a sub-Planckian field excursion. We explicitly demonstrate the testability of our mechanism with upcoming cosmic microwave background B-mode observations.

关键词： Cosmic microwave background Gravitational wave sources Inflation

Gravitational waves from primordial black hole isocurvature: the effect of non-Gaussianities

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Journal of cosmology and Astroparticle physics 2024年第12期2024卷 039页

作者： He, Xin-Chen Cai, Yi-Fu Ma, Xiao-Han Papanikolaou, Theodoros Saridakis, Emmanuel N. Sasaki, Misao Department of Astronomy School of Physical Sciences University of Science and Technology of China Anhui Hefei 230026 China CAS Key Laboratory for Research in Galaxies and Cosmology School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei 230026 China Deep Space Exploration Laboratory Hefei 230088 China Scuola Superiore Meridionale Largo San Marcellino 10 Napoli 80138 Italy Istituto Nazionale di Fisica Nucleare (INFN) Sezione di Napoli Via Cinthia 21 Napoli 80126 Italy National Observatory of Athens Lofos Nymfon Athens 11852 Greece Departamento de Matemáticas Universidad Católica del Norte Avda. Angamos 0610 Casilla Antofagasta 1280 Chile Kavli Institute for the Physics and Mathematics of the Universe (WPI) UTIAS The University of Tokyo Chiba Kashiwa 277-8583 Japan Center for Gravitational Physics Yukawa Institute for Theoretical Physics Kyoto University Kyoto 606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei 10617 Taiwan

Ultra-light primordial black holes (PBHs) with masses M PBH 8g can dominate transiently the energy budget of the Universe and reheat the Universe through their evaporation taking place before Big Bang Nucleosynthesis.... 详细信息

Ultra-light primordial black holes (PBHs) with masses M _PBH < 5 × 10⁸g can dominate transiently the energy budget of the Universe and reheat the Universe through their evaporation taking place before Big Bang Nucleosynthesis. The isocurvature energy density fluctuations associated to the inhomogeneous distribution of a population of such PBHs can induce an abundant production of GWs due to second-order gravitational effects. In this work, we discuss the effect of primordial non-Gaussianity on the clustering properties of PBHs and study the effect of a clustered PBH population on the spectral shape of the aforementioned induced GW signal. In particular, focusing on local-type non-Gaussianity we find a double-peaked GW signal with the amplitude of the low-frequency peak being proportional to the square of the non-Gaussian parameter τ _NL. Remarkably, depending on the PBH mass M _PBH and the initial abundance of PBHs at formation time, i.e. Ω_PNH,f, this double-peaked GW signal can lie well within the frequency bands of forthcoming GW detectors, namely LISA, ET, SKA and BBO, hence rendering this signal falsifiable by GW experiments and promoting it as a novel portal probing the primordial non-Gaussianity. © 2024 IOP Publishing Ltd and Sissa Medialab. All rights, including for text and data mining, AI training, and similar technologies, are reserved.

关键词： gravitational waves / theory inflation physics of the early universe primordial black holes

Efficient State Preparation for the Schwinger Model with a Theta Term

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arXiv 2024年

作者： Bazavov, Alexei Henke, Brandon Hostetler, Leon Lee, Dean Lin, Huey-Wen Pederiva, Giovanni Shindler, Andrea Department of Computational Mathematics Science Michigan State University East LansingMI48824 United States Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Physics Indiana University BloomingtonIN47405 United States Facility for Rare Isotope Beams Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Jülich Supercomputing Center Forschungszentrum Jülich Wilhelm-Johnen-Straße Jülich54245 Germany Forschungszentrum Jülich Wilhelm-Johnen-Straße Jülich52425 Germany Institute for Theoretical Particle Physics and Cosmology TTK RWTH Aachen University Sommerfeldstr. 16 Aachen52074 Germany Nuclear Science Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics University of California BerkeleyCA94720 United States

We present a comparison of different quantum state preparation algorithms and their overall efficiency for the Schwinger model with a theta term. While adiabatic state preparation (ASP) is proved to be effective, in practice it leads to large CNOT gate counts to prepare the ground state. The quantum approximate optimization algorithm (QAOA) provides excellent results while keeping the CNOT counts small by design, at the cost of an expensive classical minimization process. We introduce a "blocked" modification of the Schwinger Hamiltonian to be used in the QAOA that further decreases the length of the algorithms as the size of the problem is increased. The rodeo algorithm (RA) provides a powerful tool to efficiently prepare any eigenstate of the Hamiltonian, as long as its overlap with the initial guess is large enough. We obtain the best results when combining the blocked QAOA ansatz and the RA, as this provides an excellent initial state with a relatively short algorithm without the need to perform any classical steps for large problem sizes. Copyright © 2024, The Authors. All rights reserved.

关键词： Hamiltonians