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Timing properties of the X-ray accreting pulsar 1A 0535+262 studied with Insight-HXMT

arXiv 2022年

作者： Wang, Peng Ju Kong, L.D. Zhang, S. Doroshenko, V. Santangelo, A. Ji, L. Yorgancioglu, E.S. Chen, Y.P. Zhang, S.N. Qu, J.L. Ge, M.Y. Li, J. Chang, Z. Tao, L. Peng, J.Q. Shui, Q.C. University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100049 China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Institut für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Tübingen72076 Germany Space Research Institute The Russian Academy of Sciences Profsoyuznaya Str. 84/32 Moscow117997 Russia School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China 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

We report results on the timing analysis of the 2020 giant outburst of 1A 0535+262, using broadband data from Insight-HXMT. The analysis of the pulse profile evolution from the sub-critical luminosity to super-critica... 详细信息

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The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way-mass Galaxies

arXiv

引用

arXiv 2024年

作者： Geha, Marla Mao, Yao-Yuan Wechsler, Risa H. Asali, Yasmeen Kado-Fong, Erin Kallivayalil, Nitya Nadler, Ethan O. Tollerud, Erik J. Weiner, Benjamin de Los Reyes, Mithi A.C. Wang, Yunchong Wu, John F. Department of Astronomy Yale University New HavenCT06520 United States Department of Physics and Astronomy University of Utah Salt Lake CityUT84112 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Department of Physics Yale Center for Astronomy & Astrophysics Yale University New HavenCT06520 United States Department of Astronomy University of Virginia CharlottesvilleVA22904 United States Carnegie Observatories 813 Santa Barbara Street PasadenaCA91101 United States Department of Physics & Astronomy University of Southern California Los AngelesCA90007 United States Space Telescope Science Institute BaltimoreMD21218 United States Department of Astronomy and Steward Observatory University of Arizona TucsonAZ85721 United States Department of Physics and Astronomy Amherst College AmherstMA01002 United States Center for Astrophysical Sciences Johns Hopkins University BaltimoreMD21218 United States

We present the star-forming properties of 378 satellite galaxies around 101 Milky Way analogs in the Satellites Around Galactic Analogs (SAGA) Survey, focusing on the environmental processes that suppress or quench st... 详细信息

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Galaxy bias in the era of LSST: perturbative bias expansions

arXiv

引用

arXiv 2023年

作者： Nicola, Andrina Hadzhiyska, Boryana Findlay, Nathan García-García, Carlos Alonso, David Slosar, Anže Guo, Zhiyuan Kokron, Nickolas Angulo, Raúl Aviles, Alejandro Blazek, Jonathan Dunkley, Jo Jain, Bhuvnesh Pellejero, Marcos Sullivan, James Walter, Christopher W. Zennaro, Matteo Argelander Institut für Astronomie Universität Bonn Auf dem Hügel 71 Bonn53121 Germany Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institute of Cosmology and Gravitation University of Portsmouth Burnaby Road PortsmouthPO1 3FX United Kingdom Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Brookhaven National Laboratory Physics Department UptonNY11973 United States Department of Physics Duke University DurhamNC27708 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA United States Kavli Institute for Particle Astrophysics and Cosmology SLAC National Accelerator Laboratory Menlo ParkCA United States Paseo Manuel de Lardizabal 4 Donostia-San Sebastián20018 Spain IKERBASQUE Basque Foundation for Science Bilbao48013 Spain Departamento de Física Instituto Nacional de Investigaciones Nucleares Apartado Postal 18-1027 Col. Escandón Ciudad de México11801 Mexico Consejo Nacional de Ciencia y Tecnología Av. Insurgentes Sur 1582 Colonia Crédito Constructor Del. Benito Juárez Ciudad de México03940 Mexico Department of Physics Northeastern University BostonMA02115 United States Department of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Department of Astrophysical Sciences Peyton Hall Princeton University PrincetonNJ08544 United States Center for Particle Cosmology Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Astronomy University of California BerkeleyCA94720 United States Berkeley Center for Cosmological Physics University of California BerkeleyCA94720 United States

Upcoming imaging surveys will allow for high signal-to-noise measurements of galaxy clustering at small scales. In this work, we present the results of the Rubin Observatory Legacy Survey of Space and Time (LSST) bias challenge, the goal of which is to compare the performance of different nonlinear galaxy bias models in the context of LSST Year 10 (Y10) data. Specifically, we compare two perturbative approaches, Lagrangian perturbation theory (LPT) and Eulerian perturbation theory (EPT) to two variants of Hybrid Effective Field Theory (HEFT), with our fiducial implementation of these models including terms up to second order in the bias expansion as well as nonlocal bias and deviations from Poissonian stochasticity. We consider a variety of different simulated galaxy samples and test the performance of the bias models in a tomographic joint analysis of LSST-Y10-like galaxy clustering, galaxy-galaxy-lensing and cosmic shear. We find both HEFT methods as well as LPT and EPT combined with non-perturbative predictions for the matter power spectrum to yield unbiased constraints on cosmological parameters up to at least a maximal scale of kmax = 0.4 Mpc−1 for all samples considered, even in the presence of assembly bias. While we find that we can reduce the complexity of the bias model for HEFT without compromising fit accuracy, this is not generally the case for the perturbative models. We find significant detections of non-Poissonian stochasticity in all cases considered, and our analysis shows evidence that small-scale galaxy clustering predominantly improves constraints on galaxy bias rather than cosmological parameters. These results therefore suggest that the systematic uncertainties associated with current nonlinear bias models are likely to be subdominant compared to other sources of error for tomographic analyses of upcoming photometric surveys, which bodes well for future galaxy clustering analyses using these high signal-to-noise data. Copyright © 2023, The Aut

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Geometrical reconstruction of fluorescence events observed by the LHAASO experiment

引用

Chinese physics C 2021年第4期45卷 416-425页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang X.C.Chang B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen X.L.Chen Y.Chen N.Cheng Y.D.Cheng S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.DEtorre Piazzoli X.J.Dong J.H.Fan Y.Z.Fan Z.X.Fan J.Fang J.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu S.Hu S.C.Hu X.J.Hu D.H.Huang Q.L.Huang W.H.Huang X.T.Huang Z.C.Huang F.Ji X.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li W.L.Li X.Li X.Li X.R.Li Y.Li Y.Z.Li Z.Li Z.Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu H.Liu H.D.Liu J.Liu J.L.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.C.Nan B.Y..Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Saiz L.Shao O.Shchegolev X.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun Z.B.Sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wang C.Wang H.Wang H.G.Wang J.C.Wang J.S.Wang L.P.Wang L.Y.Wang R.N.Wang W.Wang W.Wang X.G.Wang X.J.Wang X.Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu S.Wu W.X.Wu X.F.Wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao H.B.Xiao G.G.Xin Y.L.Xin Y.Xing D.L.Xu R.X.Xu L.Xue D.H.Yan C.W.Yang F.F.Yang J.Y.Yang L.L.Yang M.J.Yang R.Z.Yang S.B.Yang Y.H.Yao Z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.W.Zhang L.Zhang L.Zhang L.X.Zhang P.F.Zhang P.F.Zhang R.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang B.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Paricle Detection and Electronics China University of Science and Technology of China HefeiAnhui 230026China Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhouGuangdong 510006China School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhaiGuangdong 519000China School of Physical Science and Technology Guangxi UniversityNanningGuangxi 530004China Hebei Normal University ShijiazhuangHebei 050024China School of Physics and Microelectronics Zhengzhou UniversityZhengzhouHenan 450001China School of Astronomy and Space Science Nanjing UniversityNanjingJiangsu 210023China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjingJiangsu 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdaoShandong 266237China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology Southwest Jiaotong UniversityChengduSichuan 610031China College of Physics Sichuan UniversityChengduSichuan 610065China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasaTibet 850000China School of physics and technology Wuhan UniversityWuhanHubei 430072Ch

The LHAASO-WFCTA experiment,which aims to observe cosmic rays in the sub-EeV range using the fluorescence technique,uses a new generation of high-performance *** ensure that the experiment has ex-cellent detection cap... 详细信息

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Excitations of Ising Strings on a Lattice

arXiv

引用

arXiv 2022年

作者： Athenodorou, Andreas Dubovsky, Sergei Luo, Conghuan Teper, Michael Computation-based Science and Technology Research Center The Cyprus Institute Cyprus Dipartimento di Fisica Universitá di Pisa INFN Sezione di Pisa Largo Pontecorvo 3 Pisa56127 Italy Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY10003 United States Rudolf Peierls Centre for Theoretical Physics Clarendon Laboratory University of Oxford Parks Road OxfordOX1 3PU United Kingdom All Souls College University of Oxford High Street OxfordOX1 4AL United Kingdom

The 3d Ising model in the low temperature (ferromagnetic) phase describes dynamics of two-dimensional surfaces—domain walls between clusters of parallel spins. The Kramers–Wannier duality maps these surfaces into wo... 详细信息

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