检索结果-内蒙古大学图书馆

Accurate and robust methods for direct background estimation in resonant anomaly detection

学校读者我要写书评

暂无评论

Physical Review D 2025年第9期111卷 094041-094041页

作者： Ranit Das Thorben Finke Marie Hein Gregor Kasieczka Michael Krämer Alexander Mück David Shih NHETC Department of Physics and Astronomy Rutgers University Piscataway New Jersey 08854 USA Institute for Theoretical Particle Physics and Cosmology RWTH Aachen University D-52056 Aachen Germany Institut für Experimentalphysik Universität Hamburg 22761 Hamburg Germany Center for Data and Computing in Natural Sciences (CDCS) 22607 Hamburg Germany

Resonant anomaly detection methods have great potential for enhancing the sensitivity of traditional bump hunt searches. A key component of these methods is a high quality background template used to produce an anomaly score. Using the LHC Olympics R&D dataset, we demonstrate that this background template can also be repurposed to directly estimate the background expectation in a simple cut and count setup. In contrast to a traditional bump hunt, no fit to the invariant mass distribution is needed, thereby avoiding the potential problem of background sculpting. Furthermore, direct background estimation allows working with large background rejection rates, where resonant anomaly detection methods typically show their greatest improvement in significance.

关键词：

X-RAY POLARIZATION OF THE MAGNETAR 1E 1841−045

学校读者我要写书评

暂无评论

arXiv 2024年

作者： Stewart, Rachael Younes, George A. Harding, Alice K. Wadiasingh, Zorawar Baring, Matthew G. Negro, Michela Strohmayer, Tod E. Ho, Wynn C.G. Ng, Mason Arzoumanian, Zaven Thi, Hoa Dinh Di Lalla, Niccolò Enoto, Teruaki Gendreau, Keith Hu, Chin-Ping Van Kooten, Alex Kouveliotou, Chryssa McEwen, Alexander Department of Physics The George Washington University WashingtonDC20052 United States Astrophysics Science Division NASA Goddard Space Flight Center GreenbeltMD20771 United States Center for Space Sciences and Technology University of Maryland Baltimore County BaltimoreMD21250 United States Theoretical Division Los Alamos National Laboratory Los AlamosNM87545 United States Department of Astronomy University of Maryland College ParkMD20742 United States Astrophysics Science Division NASA Goddard Space Flight Center GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA/GSFC GreenbeltMD20771 United States Department of Physics and Astronomy - MS 108 Rice University 6100 Main Street HoustonTX77251-1892 United States Department of Physics & Astronomy Louisiana State University Baton RougeLA70803 United States Department of Physics and Astronomy Haverford College 370 Lancaster Avenue Haverford PA19041 United States Department of Physics McGill University 3600 rue University MontréalQCH3A 2T8 Canada Trottier Space Institute McGill University 3550 rue University MontréalQCH3A 2A7 Canada Astrophysics Science Division NASA Goddard Space Flight Center GreenbeltMD20771 United States W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States RIKEN Cluster for Pioneering Research 2-1 Hirosawa Saitama Wako351-0198 Japan Department of Physics National Changhua University of Education Changhua50007 Taiwan

We report on IXPE and NuSTAR observations beginning forty days after the 2024 outburst onset of magnetar 1E 1841-045, marking the first IXPE observation of a magnetar in an enhanced state. Our spectropolarimetric analysis indicates that both a blackbody (BB) plus double power-law (PL) and a double blackbody plus power-law spectral model fit the phase-averaged intensity data well, with a hard PL tail (Γ = 1.19 and 1.35, respectively) dominating above ≈ 5 keV. For the former model, we find the soft PL (the dominant component at soft energies) exhibits a polarization degree (PD) of ≈ 30% while the hard PL displays a PD of ≈ 40%. Similarly, the cool BB of the 2BB+PL model possesses a PD of ≈ 15% and a hard PL PD of ≈ 57%. For both models, each component has a polarization angle (PA) compatible with celestial north. Model-independent polarization analysis supports these results, wherein the PD increases from ≈ 15% to ≈ 70% in the 2–3 keV and 6–8 keV ranges, respectively, while the PA remains nearly constant. We find marginal evidence for phase-dependent variability of the polarization properties, namely a higher PD at phases coinciding with the hard X-ray pulse peak. We compare the hard X-ray PL to the expectation from resonant inverse Compton scattering (RICS) and secondary pair cascade synchrotron radiation from primary high-energy RICS photons;both present reasonable spectropolarimetric agreement with the data, albeit, the latter more naturally. We suggest that the soft PL X-ray component may originate from a Comptonized corona in the inner magnetosphere. © 2024, CC BY.

关键词： Compton scattering

Chiral phase structure of the sixteen meson states in the SU(3) Polyakov linear-sigma model for finite temperature and chemical potential in a strong magnetic field

学校读者我要写书评

暂无评论

Chinese physics C 2019年第3期43卷 56-71页

作者： Abdel Nasser Tawfik Abdel Magied Diab M.T.Hussein Nile University Juhayna sq.of 26th-July-Corridor16453 GizaEgypt Frankfurt Institute for Advanced Studies Ruth Moufang Str.160438 FrankfurtGermany and World Laboratory for Cosmology And Particle Physics(WLCAPP)11571 CairoEgypt Egyptian Center for Theoretical Physics(ECTP) MTI University11571 CairoEgypt and World Laboratory for Cosmology And Particle Physics(WLCAPP)11571 CairoEgypt Physics Department Faculty of ScienceCairo University12613 GizaEgypt

In characterizing the chiral phase-structure of pseudoscalar(J^(pc) = 0^(-+)), scalar(J^(pc) = 0^(++)), vector(J^(pc) =1^(--)) and axial-vector(J^(pc) = 1^(++)t) meson states and their dependence on temperature, chemical potential, and magnetic field,we utilize the SU(3) Polyakov linear-sigma model(PLSM) in the mean-field approximation. We first determine the chiral(non)strange quark condensates,σ_l and σ_s, and the corresponding deconfinement order parameters, φ and φ~*, in thermal and dense(finite chemical potential) medium and finite magnetic field. The temperature and the chemical potential characteristics of nonet meson states normalized to the lowest bosonic Matsubara frequency are analyzed. We note that all normalized meson masses become temperature independent at different critical temperatures. We observe that the chiral and deconfinement phase transitions are shifted to lower quasicritical temperatures with increasing chemical potential and magnetic field. Thus, we conclude that the magnetic field seems to have almost the same effect as the chemical potential, especially on accelerating the phase transition, i.e. inverse magnetic catalysis. We also find that increasing the chemical potential enhances the mass degeneracy of the various meson masses, while increasing the magnetic field seems to reduce the critical chemical potential, at which the chiral phase transition takes place. Our mass spectrum calculations agree well with the recent PDG compilations and PNJL, lattice QCD calculations, and QMD/UrQMD simulations.

关键词： Chiral transition magnetic fields magnetic catalysis critical temperature viscous properties of QGP

Self-calibration of photometric redshift scatter from DECaLS DR8 power spectrum and validation with simulated catalogues

学校读者我要写书评

暂无评论

arXiv 2022年

作者： Peng, Hui Xu, Haojie Zhang, Le Chen, Zhao Yu, Yu Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University 800 Dongchuan Road Shanghai200240 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China School of Physics and Astronomy Sun Yat-Sen University 2 Daxue Road Zhuhai519082 China CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area Zhuhai519082 China Peng Cheng Laboratory No.2 Xingke 1st Street Shenzhen518000 China

The uncertainty in the photometric redshift estimation is one of the major systematics in weak lensing cosmology. The self-calibration method is able to reduce this systematics without assuming strong priors. We improve the recently proposed self-calibration algorithm to enhance the stability and robustness with the noisy measurement. The improved algorithm is tested on the power spectra measured from the simulated catalogues constructed according to DECaLS DR8 photometric catalogue. For the fiducial analysis with 5 equal-width redshift bins over 0 Copyright © 2022, The Authors. All rights reserved.

关键词： Power spectrum

Observations of the Cabibbo-Suppressed decays Λ_(c)^(+)→nπ+π^(0),nπ^(+)π^(-)π^(+) and the Cabibbo-Favored decay Λ_(c)^(+)→nK^(-)π^(+)π^(+)

学校读者我要写书评

暂无评论

Chinese physics C 2023年第2期47卷 1-18页

作者：麦迪娜 M.N.Achasov P.Adlarson M.Albrecht R.Aliberti A.Amoroso 安美儒安琪白羽 O.Bakina R.Baldini Ferroli I.Balossino 班勇 V.Batozskaya D.Becker K.Begzsuren N.Berger M.Bertani D.Bettoni F.Bianchi E.Bianco J.Bloms A.Bortone I.Boyko R.A.Briere A.Brueggemann 蔡浩蔡啸 A.Calcaterra 曹国富曹宁 S.A.Cetin 常劲帆常万玲车国荣 G.Chelkov 陈琛陈超陈刚陈和生陈玛丽陈申见陈少敏 T.Chen 陈旭荣 X.T.Chen 陈元柏陈卓俊成伟帅 S.K.Choi 初晓 G.Cibinetto F.Cossio 崔佳佳代洪亮代建平 A.Dbeyssi R.Ede Boer D.Dedovich 邓子艳 A.Denig I.Denysenko M.Destefanis F.De Mori 丁勇丁逸董静董燎原董明义董翔杜书先段宗欢 P.Egorov 范玉兰方建房双世方文兴方易 R.Farinelli L.Fava F.Feldbauer G.Felici 封常青冯俊华 K Fischer M.Fritsch C.Fritzsch 傅成栋高涵高原宁高扬 S.Garbolino I.Garzia 葛潘婷葛振武耿聪 E.M.Gersabeck A Gilman K.Goetzen 龚丽龚文煊 W.Gradl M.Greco 谷立民顾旻皓顾运厅关春懿郭爱强郭立波郭如盼郭玉萍 A.Guskov 韩文颖郝喜庆 F.A.Harris 何凯凯何康林 F.H.Heinsius C.H.Heinz 衡月昆 C.Herold 侯国一侯颖锐侯治龙胡海明 J.F.Hu 胡涛胡誉黄光顺黄凯旋黄麟钦黄性涛黄燕萍黄震 T.Hussain N Hüsken W.Imoehl M.Irshad J.Jackson S.Jaeger S.Janchiv E.Jang J.H.Jeong 纪全姬清平季晓斌季筱璐吉钰瑶贾泽坤姜赛赛江晓山 Y.Jiang 焦健斌焦铮金山金毅荆茂强 T.Johansson N.Kalantar-Nayestanaki 康晓珅 R.Kappert M.Kavatsyuk 柯百谦 I.K.Keshk A.Khoukaz R.Kiuchi R.Kliemt L.Koch O.B.Kolcu B.Kopf M.Kuemmel M.Kuessner A.Kupsc W.Kühn J.J.Lane J.S.Lange P.Larin A.Lavania L.Lavezzi 雷祚弘 H.Leithoff M.Lellmann T.Lenz 李翠李聪李春花李澄李德民李飞李刚李慧李贺李海波李惠静 H.N.Li J.Q.Li 李静舒李井文李科 L.J Li 李龙科李蕾李明浩李培荣李素娴栗帅迎李腾李卫东李卫国李旭红李晓玲李晓宇李彦谷李振轩李紫源梁畅梁昊梁浩梁浩梁勇飞梁羽铁廖广睿廖龙洲 J.Libby A.Limphirat 林创新林德旭 T.Lin 刘北江刘成刘春秀 D.Liu 刘福虎刘芳刘峰 G.M.Liu H.Liu 刘宏邦刘怀民刘欢欢刘汇慧刘建北刘佳俊刘晶译刘凯刘魁勇刘珂刘亮刘露刘美宏刘佩莲刘倩刘树彬刘桐刘维克刘卫民刘翔刘英刘玉斌刘振安刘智青娄辛丑卢飞翔吕海江吕军光陆小玲卢宇卢云鹏 Z.H.Lu 罗成林罗民兴罗涛罗小兰吕晓睿吕翌丰马凤才马海龙马连良马明明马秋梅马润秋马瑞廷马骁妍马尧 F.E.Maas M.Maggiora S.Maldaner S.Malde Q.A.Malik A.Mangoni 冒亚军毛泽普 S.Marcello 孟召霞 J.G.Messchendorp G.Mezzadri H.Miao 闵天觉 R.E.Mitchell 莫晓虎 N.Yu.Muchnoi Y.Nefedov F.Nerling I.B.Nikolaev 宁哲 S.Nisar 牛艳 S.L.Olsen 欧阳群 S.Pacetti 潘祥潘越 A.Pathak P.Patteri M.Pelizaeus 彭海平 K.Peters 平加伦平荣刚 S.Plura S.Pogodin V.Prasad 齐法制齐航漆红荣祁鸣齐天钰钱森钱文斌钱圳乔从丰秦佳佳秦丽清覃潇平秦小帅秦中华邱进发屈三强 K.H.Rashid C.F Institute of High Energy Physics Beijing 100049China Beihang University Beijing 100191China Beijing Institute of Petrochemical Technology Beijing 102617China Bochum Ruhr-University D-44780 BochumGermany Carnegie Mellon University PittsburghPennsylvania 15213USA Central China Normal University Wuhan 430079China Central South University Changsha 410083China China Center of Advanced Science and Technology Beijing 100190China COMSATS University Islamabad Lahore CampusDefence RoadOff Raiwind Road54000 LahorePakistan Fudan University Shanghai 200433China G.I.Budker Institute of Nuclear Physics SB RAS(BINP) Novosibirsk 630090Russia GSI Helmholtzcentre for Heavy Ion Research GmbH D-64291 DarmstadtGermany Guangxi Normal University Guilin 541004China Guangxi University Nanning 530004China Hangzhou Normal University Hangzhou 310036China Hebei University Baoding 071002China Helmholtz Institute Mainz Staudinger Weg 18D-55099 MainzGermany Henan Normal University Xinxiang 453007China Henan University of Science and Technology Luoyang 471003China Henan University of Technology Zhengzhou 450001China Huangshan College Huangshan 245000China Hunan Normal University Changsha 410081China Hunan University Changsha 410082China Indian Institute of Technology Madras Chennai 600036India Indiana University BloomingtonIndiana 47405USA INFN Laboratori Nazionali di Frascati I-00044FrascatiItaly INFN Sezione di Perugia I-06100PerugiaItaly University of Perugia I-06100PerugiaItaly INFN Sezione di Ferrara I-44122FerraraItaly University of Ferrara I-44122FerraraItaly Institute of Modern Physics Lanzhou 730000China Institute of Physics and Technology Peace Avenue 54BUlaanbaatar 13330Mongolia Jilin University Changchun 130012China Johannes Gutenberg University of Mainz Johann-Joachim-Becher-Weg 45D-55099 MainzGermany Joint Institute for Nuclear Research 141980 DubnaMoscow regionRussia Justus-Liebig-Universitaet Giessen II.Physikalisches InstitutHeinrich-Buff-Ring 16D-35392 GiessenGermany Lanzhou Un

Using electron-positron annihilation data samples corresponding to an integrated luminosity of 4.5 fb-1,collected by the BESⅢdetector in the energy region between 4599.53 MeV and 4698.82 MeV,we report the first observations of the Cabibbo-suppressed decaysΛ_(c)^(+)→nπ^(+)π^(0),Λ_(c)^(+)→nπ^(+)π^(-)π^(+),and the Cabibbo-favored decayΛ_(c)^(+)→nK^(-)π^(+)π^(+)with statistical significances of 7.9σ,7.8σ,and>10σ,*** branching fractions of these decays are measured to be B(Λ_(c)^(+)→nπ^(+)π^(0))=(0.64±0.09±0.02)%,B(Λ_(c)^(+)→nπ^(+)π^(-)π^(+))=(0.45±0.07±0.03)%,and B(Λ_(c)^(+)→nK^(-)π^(+)π^(+))=(1.90±0.08±0.09)%,where the first uncertainties are statistical and the second are *** find that the branching fraction of the decayΛ_(c)^(+)→nπ^(+)π^(0)is about one order of magnitude higher than that ofΛ_(c)^(+)→nπ^(+).

关键词： ∧_(c)^(+)baryon Branching fraction BESⅢdetector

The Early Evolution of Magnetar Rotation I: Slowly Rotating "Normal" Magnetars

学校读者我要写书评

暂无评论

arXiv 2022年

作者： Prasanna, Tejas Coleman, Matthew S.B. Raives, Matthias J. Thompson, Todd A. Department of Physics The Ohio State University ColumbusOH43210 United States Center for Cosmology & Astro-Particle Physics The Ohio State University ColumbusOH43210 United States Department of Astrophysical Sciences PrincetonNJ08540 United States Department of Astronomy The Ohio State University ColumbusOH43210 United States The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States

In the seconds following their formation in core-collapse supernovae, "proto"-magnetars drive neutrino-heated magneto-centrifugal winds. Using a suite of two-dimensional axisymmetric MHD simulations, we show that relatively slowly rotating magnetars with initial spin periods of p★0 = 50 − 500 ms spin down rapidly during the neutrino Kelvin-Helmholtz cooling epoch. These initial spin periods are representative of those inferred for normal Galactic pulsars, and much slower than those invoked for gamma-ray bursts and super-luminous supernovae. Since the flow is non-relativistic at early times, and because the Alfvén radius is much larger than the proto-magnetar radius, spindown is millions of times more efficient than the typically-used dipole formula. Quasi-periodic plasmoid ejections from the closed zone enhance spindown. For polar magnetic field strengths b0 & 5×1014 G, the spindown timescale can be shorter than than the Kelvin-Helmholtz timescale. For B0 & 1015 G, it is of order seconds in early phases. We compute the spin evolution for cooling proto-magnetars as a function of B0, P★0, and mass (M). Proto-magnetars born with B0 greater than ' 1.3 × 1015 G (P★0/400 ms)−1.4(M/1.4 M)2.2 spin down to periods > 1 s in just the first few seconds of evolution, well before the end of the cooling epoch and the onset of classic dipole spindown. Spindown is more efficient for lower M and for larger P★0. We discuss the implications for observed magnetars, including the discrepancy between their characteristic ages and supernova remnant ages. Finally, we speculate on the origin of 1E 161348-5055 in the remnant RCW 103, and the potential for other ultra-slowly rotating magnetars. Copyright © 2022, The Authors. All rights reserved.

关键词： Cooling

Search for Dark-Matter-Nucleon Interactions with a Dark Mediator in PandaX-4T

学校读者我要写书评

暂无评论

arXiv 2023年

作者： Huang, Di 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, 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 Ning, Xuyang 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 Huo, Ran Yu, Haibo Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai200240 China 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 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 of 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

We report results of a search for dark-matter-nucleon interactions via a dark mediator using optimized low-energy data from the PandaX-4T liquid xenon experiment. With the ionization-signal-only data and utilizing the Migdal effect, we set the most stringent limits on the cross section for dark matter masses ranging from 30 MeV/c2 to 2 GeV/c2. Under the assumption that the dark mediator is a dark photon that decays into scalar dark matter pairs in the early Universe, we rule out significant parameter space of such thermal relic dark-matter model. Copyright © 2023, The Authors. All rights reserved.

关键词： Dark Matter

Hybrid stars can be self-bound

学校读者我要写书评

暂无评论

Physical Review D 2021年第9期103卷 094037-094037页

作者： Li-Qun Su Chao Shi Yong-Feng Huang Yan Yan Cheng-Ming Li Hongshi Zong Department of physics Nanjing University Nanjing 210093 China Department of Nuclear Science and Technology Nanjing University of Aeronautics and Astronautics Nanjing 210016 China School of Astronomy and space science Nanjing University Nanjing 210023 China School of Mathematics and physics Changzhou University Changzhou 213164 China School of physics and Microelectronics Zhengzhou University Zhengzhou 450001 China Department of physics Anhui Normal University Wuhu 241000 China Nanjing Proton Source Research and Design Center Nanjing 210093 China Joint Center for Particle Nuclear Physics and Cosmology Nanjing 210093 China

Based on the properties of uniform nuclear matter at the nuclear saturation density and basic thermodynamic relations, we first restudy the composition of matter on the surface of normal neutron stars and hybrid stars. It is found that hybrid stars are composed of uniform hadronic matter on the surface rather than heavy nuclei. Then we use the Walecka model and the self-consistent NJL model to describe the equation of state of low-density hadrons and quark matter at high densities respectively. The P-interpolation method is employed to connect the equation of state at the extreme densities to study hybrid stars. As a result, we find that the obtained hybrid star mass-radius relation and tidal deformability meet the requirements of the latest astronomical data. More importantly, we find that the hybrid stars we obtained can be self-bound rather than gravitationally bound, which is completely different from previous related studies.

关键词： Nuclear matter in neutron stars Strong interaction

Core to Cosmic Edge: SIMBA-C’s New Take on Abundance Profiles in the Intragroup Medium at z = 0

学校读者我要写书评

暂无评论

arXiv 2025年

作者： Padawer-Blatt, Aviv Shao, Zhiwei Hough, Renier T. Rennehan, Douglas Barré, Ruxin Saeedzadeh, Vida Babul, Arif Davé, Romeel Kobayashi, Chiaki Cui, Weiguang Mernier, François Gozaliasl, Ghassem Department of Physics and Astronomy University of Victoria VictoriaBCV8P 1A1 Canada Department of Astronomy School of Physics and Astronomy Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai Jiao Tong University Shanghai200240 China Center for Space Research North-West University Potchefstroom2520 South Africa Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Department of Physics & Astronomy Johns Hopkins University BaltimoreMD21218 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Department of Physics Indian Institute of Science Bangalore560012 India Department of Physics University of Helsinki P.O. Box 64 HelsinkiFI-00014 Finland Centre for Astrophysics Research Department of Physics Astronomy and Mathematics University of Hertfordshire HatfieldAL10 9AB United Kingdom Departamento de Física Téorica Universidad Autónoma de Madrid MadridE-28049 Spain Universidad Autónoma de Madrid Madrid28049 Spain NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Astronomy University of Marlyand College ParkMD20742 United States Department of Computer Science Aalto University P.O. Box 15400 EspooFI-00 076 Finland

We employ the SIMBA-C cosmological simulation to study the impact of its upgraded chemical enrichment model (Chem5) on the distribution of metals in the intragroup medium (IGrM). We investigate the projected X-ray emission-weighted abundance profiles of key elements over two decades in halo mass (1013 ≤ M500/M☉ ≤ 1015). Typically, SIMBA-C generates lower-amplitude abundance profiles than SIMBA with flatter cores, in better agreement with observations. For low-mass groups, both simulations over-enrich the IGrM with Si, S, Ca, and Fe compared to observations, a trend likely related to inadequate modeling of metal dispersal and mixing. We analyze the 3D mass-weighted abundance profiles, concluding that the lower SIMBA-C IGrM abundances are primarily a consequence of fewer metals in the IGrM, driven by reduced metal yields in Chem5, and the removal of the instantaneous recycling of metals approximation employed by SIMBA. Additionally, an increased IGrM mass in low-mass SIMBA-C groups is likely triggered by changes to the AGN and stellar feedback models. Our study suggests that a more realistic chemical enrichment model broadly improves agreement with observations, but physically motivated sub-grid models for other key processes, like AGN and stellar feedback and turbulent diffusion, are required to realistically reproduce observed group environments. © 2025, CC BY.

关键词： cosmology