The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray Observable-to-Mass-and-Redshift Relations of Galaxy Clusters and Groups with Weak-Lensing Mass Calibration from the Hyper Suprime-Cam Subaru Strategic Program Survey
I-Non Chiu, Vittorio Ghirardini, Ang Liu, Sebastian Grandis, Esra Bulbul, Y. Emre Bahar, Johan Comparat, Sebastian Bocquet, Nicolas Clerc, Matthias Klein, Teng … 展开作者
I-Non Chiu, Vittorio Ghirardini, Ang Liu, Sebastian Grandis, Esra Bulbul, Y. Emre Bahar, Johan Comparat, Sebastian Bocquet, Nicolas Clerc, Matthias Klein, Teng Liu, Xiangchong Li, Hironao Miyatake, Joseph Mohr, Masamune Oguri, Nobuhiro Okabe, Florian Pacaud, Miriam E. Ramos-Ceja, Thomas H. Reiprich, Tim Schrabback, Keiichi Umetsu
备注：
Accepted for publication in A&A. Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission
We present the first weak-lensing mass calibration and X-ray scaling relations of galaxy clusters and groups selected in the $eROSITA$ Final Equatorial Depth Survey (eFEDS) observed by Spectrum Roentgen Gamma/$eROSITA$ over a contiguous footprint with an area of $\approx140$ deg$^2$, using the three-year (S19A) weak-lensing data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. In this work, a sample of $434$ optically confirmed galaxy clusters (and groups) at redshift $0.01\lesssim z \lesssim1.3$ with a median of $0.35$ is studied, of which $313$ systems are uniformly covered by the HSC survey to enable the extraction of the weak-lensing shear observable. In a Bayesian population modelling, we perform a blind analysis for the weak-lensing mass calibration by simultaneously modelling the observed count rate $η$ and the shear profile $g$ of individual clusters through the count rate-to-mass-and-redshift ($η$--$M_{500}$--$z$) and weak-lensing mass-to-mass-and-redshift ($M_{\mathrm{WL}}$--$M_{500}$--$z$) relations, respectively, while accounting for the bias in these observables using simulation-based calibrations. As a result, the count rate-inferred and lensing-calibrated cluster mass is obtained from the joint modelling of the scaling relations, as the ensemble mass spanning a range of $10^{13}h^{-1}M_{\odot}\lesssim M_{500}\lesssim10^{15} h^{-1}M_{\odot}$ with a median of $\approx10^{14} h^{-1}M_{\odot}$ for the eFEDS sample. With the mass calibration, we further model the X-ray observable-to-mass-and-redshift relations, including the rest-frame soft-band and bolometric luminosity ($L_{\mathrm{X}}$ and $L_{\mathrm{b}}$), the emission-weighted temperature $T_{\mathrm{X}}$, the mass of intra-cluster medium $M_{\mathrm{g}}$, and the mass proxy $Y_{\mathrm{X}}$, which is the product of $T_{\mathrm{X}}$ and $M_{\mathrm{g}}$. (abridged)
The eROSITA Final Equatorial-Depth Survey (eFEDS): A complete census of X-ray properties of Subaru Hyper Suprime-Cam weak lensing shear-selected clusters in the eFEDS footprint
The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray stacking analysis of Subaru's optically selected clusters spanning low richness regime
Institut für Astronomie und Astrophysik Tübingen (IAAT), Universität Tübingen（蒂宾根大学天文与天体物理研究所）；Department of Physics, Nara Women’s University（奈良女子大学理学部）；Argelander-Institut für Astronomie (AIfA), Universität Bonn（波恩大学阿尔兰德天体物理研究所）；Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University（广岛大学先进理工学研究科物理学项目）；Hiroshima Astrophysical Science Center, Hiroshima University（广岛大学广岛天体科学中心）；Core Research for Energetic Universe, Hiroshima University（广岛大学宇宙高能前沿核心研究）；Center for Frontier Science, Chiba University（千叶大学前沿科学中心）；Department of Physics, Graduate School of Science, Chiba University（千叶大学理学研究科物理学系）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), University of Tokyo（东京大学宇宙物质数学研究所）；Graduate School of Science, Division of Particle and Astrophysical Science, Nagoya University（名古屋大学理学研究科粒子与天体物理学专业）
The eROSITA Final Equatorial Depth Survey (eFEDS): X-ray emission around star-forming and quiescent galaxies at $0.05<z<0.3$
我们的目标是在一个大样本的星系的环银河系介质的热相的特征。我们堆叠X射线事件从SRG/eROSITA eFEDS调查周围的中央星系在GAMA 9小时领域，以构建径向投影软X射线光度分布作为其恒星质量和特定的恒星形成率的函数。我们考虑恒星质量范围为$2\times 10^{10}$-$10^{12}$ M $_\odot$（$3\times 10^9$ -$6\times10^{11}$ M $_\odot$）的静止（恒星形成）星系的样本。对于静止的星系，X射线轮廓明显地扩展到整个可用的质量范围;然而，由于投影效应，测量的轮廓可能偏高，因为这些星系往往生活在稠密和炎热的环境中。对于质量最大的恒星形成样本（$\geq10^{11}$ M $_\odot$），有一个延伸发射的检测提示。对于$< 10^{11}$ M $_\odot$的恒星形成星系的X射线叠加配置文件是兼容的未解决的来源，并符合预期的发射从微弱的活动星系核和X射线双星。首次测量了静止星系和恒星形成星系的平均X射线光度与恒星质量之间的平均关系。高质量（$\geq 10^{11}$ M $_\odot$）恒星形成或静止星系遵循预期的维里化热晕的缩放，而低质量恒星形成星系显示出不太突出的光度和较弱的依赖于恒星质量，与弱活动星系核人口的经验模型一致。当比较我们的结果与国家的最先进的数值模拟，我们发现一个整体的一致性大（$>80$ …
The SRG/eROSITA All-Sky Survey. The Weak-Lensing Mass Calibration and the Stellar Mass-to-Halo Mass Relation from the Hyper Suprime-Cam Subaru Strategic Program
Cosmology with galaxy clusters using machine learning. Application to eROSITA Data
University Federico II（那不勒斯费德里科二世大学）；School of Physics and Astronomy, Sun Yat-sen University（中山大学物理与天文学院）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Scuola Superiore Meridionale（南方高等学院）；Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；CNRS（法国国家科学研究中心）；Grenoble INP（格勒诺布尔国立理工学院）；LPSC-IN2P3（粒子与核物理实验室）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München（慕尼黑大学物理学院大学天文台）；Institut für Theoretische Physik, Universität Heidelberg（海德堡大学理论物理研究所）
How the cool-core population transitions from galaxy groups to massive clusters: A comparison of the largest Magneticum simulation with eROSITA, XMM-Newton, Chandra and LOFAR observations
The SRG/eROSITA all-sky survey: Constraints on Ultra-light Axion Dark Matter through Galaxy Cluster Number Counts
Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Universität Innsbruck, Institut für Astro- und Teilchenphysik（因斯布鲁克大学天体与粒子物理研究所）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所空间科学与天文观测台）；Department of Physics and Astronomy, Stony Brook University（纽约州立大学石溪分校物理与天文学系）；Universität Hamburg, Hamburger Sternwarte（汉堡大学汉堡天文台）；Department of Physics, National Cheng Kung University（国立成功大学物理系）；IRAP, Université de Toulouse, CNRS, UPS, CNES（图卢兹大学宇宙射线与天体物理学研究所）
XMM-Newton observations of ten high-redshift CAMIRA clusters of galaxies
Nara Women’s University（奈良女子大学）；Universität Bonn（波恩大学）；Nagoya University（名古屋大学）；Hiroshima University（广岛大学）；Chiba University（千叶大学）；Ritsumeikan University（立命馆大学）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）
Baryonification IV: Constraining baryonic feedback with X-ray gas fractions
ETH Zurich（苏黎世联邦理工学院）；The University of Manchester（曼彻斯特大学）；University of Zurich（苏黎世大学）；Stockholm University（斯德哥尔摩大学）；University of Groningen（格罗宁根大学）；Universität Bonn（波恩大学）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Ludwig-Maximilians-Universität（慕尼黑大学）；CNES（法国国家空间研究中心）；IRAP（天体物理学研究所在）；Beijing Normal University（北京师范大学）
