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First Search for the Absorption of Fermionic Dark Matter with the PandaX-4T Experiment

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Physical Review Letters 2022年第16期129卷 161803-161803页

作者： Linhui Gu Abdusalam Abdukerim Zihao Bo Wei Chen Xun Chen Yunhua Chen Chen Cheng Yunshan Cheng Zhaokan Cheng Xiangyi Cui Yingjie Fan Deqing Fang Changbo Fu Mengting Fu Lisheng Geng Karl Giboni Xuyuan Guo Ke Han Changda He Jinrong He Di Huang Yanlin Huang Zhou Huang Ruquan Hou Xiangdong Ji Yonglin Ju Chenxiang Li Jiafu Li Mingchuan Li Shu Li Shuaijie Li Qing Lin Jianglai Liu Xiaoying Lu Lingyin Luo Yunyang Luo Wenbo Ma Yugang Ma Yajun Mao Nasir Shaheed Yue Meng Xuyang Ning Ningchun Qi Zhicheng Qian Xiangxiang Ren Changsong Shang Xiaofeng Shang Guofang Shen Lin Si Wenliang Sun Andi Tan Yi Tao Anqing Wang Meng Wang Qiuhong Wang Shaobo Wang Siguang Wang Wei Wang Xiuli Wang Zhou Wang Yuehuan Wei Mengmeng Wu Weihao Wu Jingkai Xia Mengjiao Xiao Xiang Xiao Pengwei Xie Binbin Yan Xiyu Yan Jijun Yang Yong Yang Yukun Yao Chunxu Yu Jumin Yuan Ying Yuan Xinning Zeng Dan Zhang Minzhen Zhang Peng Zhang Shibo Zhang Shu Zhang Tao Zhang Yuanyuan Zhang Li Zhao Qibin Zheng Jifang Zhou Ning Zhou Xiaopeng Zhou Yong Zhou Yubo Zhou School of Physics and Astronomy Shanghai Jiao Tong University Key Laboratory for Particle Astrophysics and Cosmology (MoE) Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai 200240 China 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 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 Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai 519082 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai 200240 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 102206 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 Physics and Microelectronics Zhengzhou University Zhengzhou Henan 450001 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 Pa

Compared with the signature of dark matter elastic scattering off nuclei, the absorption of fermionic dark matter by nuclei opens up a new searching channel for light dark matter with a characteristic monoenergetic signal. In this Letter, we explore the 95.0-day data from the PandaX-4T commissioning run and report the first dedicated searching results of the fermionic dark matter absorption signal through a neutral current process. No significant signal was found, and the lowest limit on the dark matter-nucleon interaction cross section is set to be 1.5×10−50 cm2 for a fermionic dark matter mass of 40 MeV/c2 with 90% confidence level.

关键词： particle dark matter Dark matter detectors

Extending the IceCube search for neutrino point sources in the Northern sky with additional years of data 38

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Extending the IceCube search for neutrino point sources in t...

38th International Cosmic Ray Conference, ICRC 2023

作者： Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Anton, G. Argüelles, C. Ashida, Y. Athanasiadou, S. Axani, S.N. Bai, X. Balagopal, A.V. Baricevic, M. Barwick, S.W. Basu, V. Bay, R. Beatty, J.J. Becker Tjus, J. Beise, J. Bellenghi, C. Benning, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Blaufuss, E. Blot, S. Bontempo, F. Book, J.Y. Boscolo Meneguolo, C. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Braun, J. Brinson, B. Brostean-Kaiser, J. Burley, R.T. Busse, R.S. Butterfield, D. Campana, M.A. Carloni, K. Carnie-Bronca, E.G. Chattopadhyay, S. Chau, N. Chen, C. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Classen, L. Coleman, A. Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Dave, P. De Clercq, C. DeLaunay, J.J. Delgado, D. Deng, S. Deoskar, K. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Domi, A. Dujmovic, H. DuVernois, M.A. Ehrhardt, T. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fang, K. Farrag, K. Fazely, A.R. Fedynitch, A. Feigl, N. Fiedlschuster, S. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Fritz, A. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goehlke, N. Gonzalez, J.G. Goswami, S. Grant, D. Gray, S.J. Gries, O. Griffin, S. Griswold, S. Groth, K.M. Günther, C. Gutjahr, P. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Hamdaoui, H. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haungs, A. Helbing, K. Hellrung, J. Henningsen, F. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hill, C. Hill, G.C. Hoffman, K.D. Hori, S. Hoshina, K. Hou, W. Huber, T. Hultqvist, K. Hünnefeld, M. Hussain, R. Hymon, K. In, S. Ishihara, A. Jacquart, M. Janik, O. Jansson, M. Japaridze, G.S. Jeong, M. III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics The International Center for Hadron Astrophysics Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute University of Copenhagen CopenhagenDK-2100 Denmark Dept. of Physics TU Dortmund University DortmundD-44221 Germany Dept. of Physics and Astro

The IceCube Neutrino Observatory is a one-cubic-kilometer-sized neutrino telescope deployed deep in the Antarctic ice at the South Pole. One of IceCube’s major goals is finding the origins of astrophysical high-energy neutrinos. In 2022, IceCube identified the strongest point-like neutrino source so far, the active galaxy NGC 1068. Analyzing 9 years of muon-neutrino data from the Northern Sky recorded between 2011 and 2020, the emission from NGC 1068 is significant at 4.2 sigma. We present a planned extension to this search with additional years of data. One of these years includes data from 2010 when IceCube was only partially constructed. We discuss the improvement in sensitivity and discovery potential for neutrino point sources across the Northern sky. We show that by building on the established analysis techniques, previous observations could be improved, not only for NGC 1068 but for all possible sources in the Northern sky. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Neutrons

Approximating new ice models with B-splines for improved IceCube event reconstruction: application to cascades and tracks 38

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Approximating new ice models with B-splines for improved Ice...

38th International Cosmic Ray Conference, ICRC 2023

作者： Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Anton, G. Argüelles, C. Ashida, Y. Athanasiadou, S. Axani, S.N. Bai, X. Balagopal, A.V. Baricevic, M. Barwick, S.W. Basu, V. Bay, R. Beatty, J.J. Becker Tjus, J. Beise, J. Bellenghi, C. Benning, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Blaufuss, E. Blot, S. Bontempo, F. Book, J.Y. Boscolo Meneguolo, C. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Braun, J. Brinson, B. Brostean-Kaiser, J. Burley, R.T. Busse, R.S. Butterfield, D. Campana, M.A. Carloni, K. Carnie-Bronca, E.G. Chattopadhyay, S. Chau, N. Chen, C. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Classen, L. Coleman, A. Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Dave, P. De Clercq, C. DeLaunay, J.J. Delgado, D. Deng, S. Deoskar, K. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Domi, A. Dujmovic, H. DuVernois, M.A. Ehrhardt, T. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fang, K. Farrag, K. Fazely, A.R. Fedynitch, A. Feigl, N. Fiedlschuster, S. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Fritz, A. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goehlke, N. Gonzalez, J.G. Goswami, S. Grant, D. Gray, S.J. Gries, O. Griffin, S. Griswold, S. Groth, K.M. Günther, C. Gutjahr, P. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Hamdaoui, H. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haungs, A. Helbing, K. Hellrung, J. Henningsen, F. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hill, C. Hill, G.C. Hoffman, K.D. Hori, S. Hoshina, K. Hou, W. Huber, T. Hultqvist, K. Hünnefeld, M. Hussain, R. Hymon, K. In, S. Ishihara, A. Jacquart, M. Janik, O. Jansson, M. Japaridze, G.S. Jeong, M. III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics The International Center for Hadron Astrophysics Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute University of Copenhagen CopenhagenDK-2100 Denmark Dept. of Physics TU Dortmund University DortmundD-44221 Germany Dept. of Physics and Astronomy M

Event signatures in IceCube are complex, modulated by both particle physics and properties of the ice and detector. Event reconstruction thus requires accurate modeling of ice properties and detector effects to fit for physics parameters, such as energy and direction. Here, we highlight how improvements in calibration can translate into substantially improving the angular resolution of electromagnetic showers. Since showers are also used to model stochastic energy losses of tracks, we further show how improved ice modeling, along with other track-specific optimizations, leads to more meaningful directional likelihood spaces for high-energy muons. The median angular resolution for showers is improved by a factor of two over an older B-spline model, and accurate directional contours for tracks can be obtained with Wilks’ theorem. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Stochastic models

Development of an in-situ calibration device of firn properties for Askaryan neutrino detectors 37

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Development of an in-situ calibration device of firn propert...

37th International Cosmic Ray Conference, ICRC 2021

作者： Beise, Jakob Glaser, Christian Anker, Astrid Baldi, Pierre Barwick, Steven W. Beise, Jakob Bernhoff, Hans Besson, Dave Z. Bingefors, Nils Cataldo, Maddalena Chen, Pisin Fernández, Daniel García Gaswint, Geoffrey Glaser, Christian Hallgren, Allan Hallmann, Steffen Hanson, Jordan C. Klein, Spencer R. Kleinfelder, Stuart A. Lahmann, Robert Liu, Jiayi Magnuson, Mitchell McAleer, Stephen Meyers, Zach Nam, Jiwoo Nelles, Anna Novikov, Alexander Paul, Manuel P. Persichilli, Christopher Plaisier, Ilse Pyras, Lilly Rice-Smith, Ryan Tatar, Joulien Wang, Shih-Hao Welling, Christoph Zhao, Leshan Uppsala University Department of Physics and Astronomy Box 516 Uppsala751 20 Sweden Department of Physics and Astronomy University of California IrvineCA92697 United States Department of Information and Computer Science University of California IrvineCA92697 United States Uppsala University Department of Physics and Astronomy UppsalaSE-752 37 Sweden Uppsala University Department of Engineering Sciences Division of Electricity UppsalaSE-752 37 Sweden Department of Physics and Astronomy University of Kansas LawrenceKS66045 United States Moscow115409 Russia ECAP Friedrich-Alexander Universität Erlangen-Nürnberg Erlangen91058 Germany Department of Physics Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan DESY Zeuthen15738 Germany Whittier College Department of Physics WhittierCA90602 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Electrical Engineering and Computer Science University of California IrvineCA92697 United States Research Cyberinfrastructure Center University of California IrvineCA92697 United States

High energy neutrinos (E >1017 eV) are detected cost-efficiently via the Askaryan effect in ice, where a particle cascade induced by the neutrino interaction produces coherent radio emission that can be picked up by antennas installed below the surface. A good knowledge of the near surface ice (aka firn) properties is required to reconstruct the neutrino properties. In particular, a continuous monitoring of the snow accumulation (which changes the depth of the antennas) and the index-of-refraction profile are crucial for an accurate determination of the neutrino’s direction and energy. We present an in-situ calibration system that extends the radio detector station with a radio emitter to continuously monitor the firn properties by measuring time differences of direct and reflected (off the surface) signals (D’n’R). We optimized the station layout in a simulation study and quantified the achievable precision. We present 14 months of data of the ARIANNA detector on the Ross Ice Shelf, Antarctica, where a prototype of this calibration system was successfully used to monitor the snow accumulation with unprecedented precision of 1 mm. We explore and test several algorithms to extract the D’n’R time difference from noisy data (including deep learning). This constitutes an in-situ test of the neutrino vertex distance reconstruction using the D’n’R technique which is needed to determine the neutrino energy. © Copyright owned by the author(s).

关键词： Ice

Spectro-polarimetry of GRB 180427A: evidence for distinct emission sites with varying polarisation

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arXiv 2025年

作者： Sonawane, Rushikesh Iyyani, Shabnam Gupta, Soumya Chattopadhyay, Tanmoy Bhattacharya, Dipankar Bhalerao, Varun B. Vadawale, Santosh V. Dewangan, G.C. Centre for High Performance Computing Indian Institute of Science Education and Research Thiruvananthapuram Thiruvananthapuram695551 India School of Physics Indian Institute of Science Education and Research Thiruvananthapuram Thiruvananthapuram695551 India Homi Bhabha National Institute Anushakti Nagar Maharashtra Mumbai400094 India Kavli Institute of Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States Department of Physics Ashoka University Haryana Sonepat131029 India Indian Institute of Technology Bombay Mumbai India Physical Research Laboratory Gujarat Ahmedabad380009 India Inter-University Center for Astronomy and Astrophysics Maharashtra Pune411007 India

The dynamics of the origin of gamma-ray emissions in gamma-ray bursts (GRBs) remains an enigma. Through a joint analysis of GRB 180427A, observed by the Fermi Gamma-ray Space Telescope and AstroSat’s Cadmium Zinc Telluride Imager, we identify emissions from two distinct regions with varying polarisation properties. Time-resolved polarisation analysis reveals a synchronous evolution of the polarisation angle (PA) and fraction (PF) with two emission pulses, peaking with a delay of 4.82 ± 0.12 s. Spectral analysis indicates that the first pulse is dominated by blackbody radiation, while the second pulse exhibits a non-thermal spectrum (power law with an exponential cutoff). Using a bottom-to-top approach through simulations, we decouple the polarisation properties of the individual spectral components, revealing polarisation fractions of 25% - 40% for the blackbody spectrum and 30% - 60% for the non-thermal spectrum. At a redshift of z ∼ 0.05, the blackbody emission originates from the jet photosphere at 1011 cm, whereas the non-thermal emission arises from an optically thin region at 1015 cm. The changing dominance of these emissions explains the observed PA shift of 60◦ ±22.3◦. The spectral cutoff at 1 MeV suggests pair opacity due to the jet’s low bulk Lorentz factor (Γ ∼ tens). The high polarisation and hard spectral slopes (α > −0.5) imply a top-hat jet structure observed off-axis, near the jet’s edge. This off-axis viewing introduces anisotropy in the radiation within the viewing cone (1/Γ), accounting for the observed polarisation. © 2025, CC BY.

关键词： Gamma rays

Robust and efficient verification of graph states in blind measurement-based quantum computation

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arXiv 2023年

作者： Li, Zihao Zhu, Huangjun Hayashi, Masahito State Key Laboratory of Surface Physics Department of Physics Fudan University Shanghai200433 China Institute for Nanoelectronic Devices and Quantum Computing Fudan University Shanghai200433 China Center for Field Theory and Particle Physics Fudan University Shanghai200433 China School of Data Science The Chinese University of Hong Kong Longgang District Shenzhen518172 China Futian District Shenzhen518048 China Graduate School of Mathematics Nagoya University Nagoya464-8602 Japan

Blind quantum computation (BQC) is a secure quantum computation method that protects the privacy of clients. Measurement-based quantum computation (MBQC) is a promising approach for realizing BQC. To obtain reliable results in blind MBQC, it is crucial to verify whether the resource graph states are accurately prepared in the adversarial scenario. However, previous verification protocols for this task are too resource consuming or noise susceptible to be applied in practice. Here, we propose a robust and efficient protocol for verifying arbitrary graph states with any prime local dimension in the adversarial scenario, which leads to a robust and efficient protocol for verifying the resource state in blind MBQC. Our protocol requires only local Pauli measurements and is thus easy to realize with current technologies. Nevertheless, it can achieve the optimal scaling behaviors with respect to the system size and the target precision as quantified by the infidelity and significance level, which has never been achieved before. Notably, our protocol can exponentially enhance the scaling behavior with the significance level. Copyright © 2023, The Authors. All rights reserved.

关键词： Quantum cryptography

Aemulus ν: precise predictions for matter and biased tracer power spectra in the presence of neutrinos

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Journal of cosmology and Astroparticle physics 2023年第7期2023卷 054页

作者： DeRose, Joseph Kokron, Nickolas Banerjee, Arka Chen, Shi-Fan White, Martin Wechsler, Risa Storey-Fisher, Kate Tinker, Jeremy Zhai, Zhongxu Physics Division Lawrence Berkeley National Laboratory 1 Cyclotron Rd CA Berkeley United States Department of Physics Stanford University 382 Via Pueblo Mall CA Stanford 94305 United States Kavli Institute for Particle Astrophysics and Cosmology SLAC National Accelerator Laboratory 2575 Sand Hill Road CA Menlo Park 94025 United States Department of Physics Indian Institute of Science Education and Research Homi Bhabha Road Pashan Pune 411008 India Institute for Advanced Study 1 Einstein Drive NJ Princeton 08540 United States Berkeley Center for Cosmological Physics Department of Physics U.C. Berkeley Campbell Hall 341 CA 94720 United States Department of Physics University of California 366 Physics North MC 7300 CA Berkeley 94720 United States Center for Cosmology and Particle Physics Department of Physics New York University 726 Broadway NY New York 10003 United States Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai 200240 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai 200240 China Waterloo Center for Astrophysics University of Waterloo Waterloo N2L 3G1 ON Canada Department of Physics and Astronomy University of Waterloo Waterloo N2L 3G1 ON Canada

We present the Aemulus ν simulations: a suite of 150 (1.05 h-1 Gpc)3 N-body simulations with a mass resolution of 3.51 × 1010 Ωcb /0.3 h-1 M ⊙ in a wνCDM cosmological parameter space. The simulations have bee... 详细信息

We present the Aemulus ν simulations: a suite of 150 (1.05 h^-1 Gpc)³ N-body simulations with a mass resolution of 3.51 × 10¹⁰ Ω_cb/0.3 h^-1 M _⊙ in a wνCDM cosmological parameter space. The simulations have been explicitly designed to span a broad range in σ ₈ to facilitate investigations of tension between large scale structure and cosmic microwave background cosmological probes. Neutrinos are treated as a second particle species to ensure accuracy to 0.5 eV, the maximum neutrino mass that we have simulated. By employing Zel'dovich control variates, we increase the effective volume of our simulations by factors of 10-10⁵ depending on the statistic in question. As a first application of these simulations, we build new hybrid effective field theory and matter power spectrum surrogate models, demonstrating that they achieve ≤ 1% accuracy for k ≤ 1 hMpc^-1 and 0 ≤ z ≤ 3, and ≤ 2% accuracy for k ≤ 4 hMpc^-1 for the matter power spectrum. We publicly release the trained surrogate models, and estimates of the surrogate model errors in the hope that they will be broadly applicable to a range of cosmological analyses for many years to come. © 2023 IOP Publishing Ltd and Sissa Medialab.

关键词： cosmological neutrinos cosmological parameters from LSS cosmological simulations dark matter simulations

Discovery of the first anti-glitch event in the rotation-powered pulsar PSR B0540-69

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arXiv 2024年

作者： Tuo, Youli Serim, Muhammed Miraç Antonelli, Marco Ducci, Lorenzo Vahdat, Armin Ge, Mingyu Santangelo, Andrea Xie, Fei Institut für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Tübingen Sand 1 Tübingen72076 Germany CNRS in2p3 Laboratoire de Physique Corpusculaire Caen14050 France ISDC Data Center for Astrophysics Université de Genève 16 chemin d'Écogia Versoix1290 Switzerland Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100049 China Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China

Using data from the Neutron star Interior Composition ExploreR (NICER) observatory, we identified a permanent spin frequency decrease of ∆ν = −(1.04 ± 0.07) × 10−7 Hz around MJD 60132 in the rotation-powered pulsar PSR B0540-69, which exhibits a periodic signal at a frequency of ν ∼ 19.6 Hz. This points to an anti-glitch event, a sudden decrease of the pulsar's rotational frequency without any major alteration in the pulse profile or any significant increase of the pulsed flux. Additionally, no burst activity was observed in association with the anti-glitch. To date, observations of the few known anti-glitches have been made in magnetars or accreting pulsars. This is the first anti-glitch detected in a rotation-powered pulsar. Given its radiatively quiet nature, this anti-glitch is possibly of internal origin. Therefore, we tentatively frame this event within a proposed mechanism for anti-glitches where the partial 'evaporation' of the superfluid component leads to an increase of the normal component's moment of inertia and a decrease of the superfluid one. © 2024, CC BY.

关键词： Rotation

New probe of non-Gaussianities with primordial black hole induced gravitational waves

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arXiv 2024年

作者： Papanikolaou, Theodoros He, Xin-Chen Ma, Xiao-Han Cai, Yi-Fu Saridakis, Emmanuel N. Sasaki, Misao Scuola Superiore Meridionale Largo San Marcellino 10 Napoli80138 Italy Sezione di Napoli Via Cinthia 21 Napoli80126 Italy National Observatory of Athens Lofos Nymfon Athens11852 Greece Department of Astronomy School of Physical Sciences University of Science and Technology of China Hefei230026 China CAS Key Laboratory for Researches in Galaxies and Cosmology School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China Deep Space Exploration Laboratory Hefei230088 China UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Departamento de Matemáticas Universidad Católica del Norte Avda. Angamos 0610 Casilla1280 Chile Center for Gravitational Physics Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan

We propose a new probe of primordial non-Gaussianities (NGs) through the observation of gravitational waves (GWs) induced by ultra-light (MPBH 9g) primordial black holes (PBHs). Interestingly enough, the existence of primordial NG can leave imprints on the clustering properties of PBHs and the spectral shape of induced GW signals. Focusing on a scale-dependent local-type NG, we identify a distinct double-peaked GW energy spectrum that, contingent upon MPBH and the abundance of PBHs at the time of formation, denoted as ΩPBH,f, may fall into the frequency bands of upcoming GW observatories, including LISA, ET, SKA, and BBO. Thus, such a signal can serve as a novel portal for probing primordial NGs. Intriguingly, combining BBN bounds on the GW amplitude, we find for the first time the joint limit on the product of the effective non-linearity parameter for the primordial tri-spectrum, denoted by τ¯NL, and the primordial curvature perturbation power spectrum PR(k), which reads as τ¯NLPR(k) −20Ω−PBH17/9f(M10PBH4g)−17/9 . Copyright © 2024, The Authors. All rights reserved.

关键词： Probes