Environmental dependence on galaxy-halo connections for satellites using HSC weak lensing
Inter-University Centre for Astronomy and Astrophysics（大学间天文学与天体物理中心）；Kavli Institute for the Physics and Mathematics of the Universe (WPI)（宇宙物理学与数学 Kavli 研究所（WPI））
We present the luminosity-halo mass relations of satellite (sLHMRs) galaxies in the SDSS redMaPPer cluster catalogue and the effects of the dense cluster environment on subhalo mass evolution. We use data from the Subaru Hyper Suprime-Cam survey Year-3 catalogue of galaxy shapes to measure the weak lensing signal around these satellites. This signal serves as a probe of the matter distribution around the satellites, thereby providing the masses of their associated subhalos. We bin our satellites based on physical observable quantities such as their luminosity or the host cluster's richness, combined with their cluster-centric radial separations. Our results indicate that although more luminous satellites tend to reside in more massive halos, the sLHMRs depend on the distance of the satellite from the cluster centre. Subhalos near the cluster centre (within $<0.3 h^{-1}Mpc$) are stripped of mass. Consequently, the ratio of subhalo mass to luminosity decreases near the cluster centre. For low luminosity galaxies ($L < 10^{10} h^{-2}L_{\odot}$), the lack of evidence of increasing subhalo masses with luminosity shows the impact of tidal stripping. We also present stellar-to-subhalo mass relations (sSHMRs) for our satellite sample evolving at different cluster-centric separations. Inferred sSHMRs in the outer radial bin appear to match that observed for the field galaxies. We show that the sSHMRs from the mock-redMaPPer run on galaxy catalogues generated by the empirical UniverseMachine galaxy formation model are in good agreement with our observational results. Satellites, when binned based on the host cluster's richness, show very little dependence of the subhalo mass on the richness.
Galaxy-Galaxy Lensing in HSC: Validation Tests and the Impact of Heterogeneous Spectroscopic Training Sets
虽然测光红移（photo-z's）是当前和即将到来的大规模调查的关键成分，高质量的光谱红移目前可用于训练，验证和测试他们是基本上不代表的幅度和颜色。我们通过跟踪来自异质训练样本的对象如何作为幅度和颜色的函数对photo-z预测做出贡献来研究这种偏差的性质和结构，并说明固定颜色下的潜在红移分布可以作为幅度的函数强烈演变。然后，我们测试的鲁棒性的星系-星系透镜信号在120度$^2$的HSC-SSP DR 1数据光谱的完整性和photo-z偏差，并发现它们的影响是次主导的当前的统计不确定性。我们的方法提供了一个框架，以调查光谱的不完整性如何影响在未来的调查，如LSST和WFIRST的照片Z为基础的弱透镜的预测。
Cosmology and Source Redshift Constraints from Galaxy Clustering and Tomographic Weak Lensing with HSC Y3 and SDSS using the Point-Mass Correction Model
Weak-lensing mass calibration of \emph{Planck} Sunyaev--Zel'dovich clusters with HSC-SSP Year~3
Stanford University（斯坦福大学）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；Princeton University（普林斯顿大学）；Nagoya University（名古屋大学）；The Inter-University Centre for Astronomy and Astrophysics（大学间天文与天体物理中心）；The University of Tokyo（东京大学）；Cornell University（康奈尔大学）；University of Pennsylvania（宾夕法尼亚大学）
First application of weak lensing peak steepness statistics to HSC Y1 data: effectively probing halo density profiles
South-Western Institute for Astronomy Research, Yunnan University（云南大学西南天文研究所）；Yunnan Key Laboratory of Survey Science, Yunnan University（云南大学云南省测绘科学重点实验室）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学与空间科学学院）；Southwest United Graduate School（西南联合研究生院）
Modelling Galaxy Clustering and Tomographic Galaxy-Galaxy Lensing with HSC Y3 and SDSS using the Point-Mass Correction Model and Redshift Self-Calibration
Simulation-Based Cosmological Mass Calibration of XXL Galaxy Clusters using HSC Weak Lensing
National Yang Ming Chiao Tung University（国立阳明交通大学）；Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理研究所）；University of Surrey（萨里大学）；University of Geneva（日内瓦大学）；École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；National Cheng Kung University（国立成功大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；INFN, Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）；Universität Bonn（波恩大学）
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
National Cheng Kung University（国立成功大学）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所空间科学天文台）；Hiroshima University（广岛大学）；Academia Sinica（中央研究院）；Chiba University（千叶大学）；National Yang Ming Chiao Tung University（国立阳明交通大学）
The suppression of the matter power spectrum: strong feedback from X-ray gas mass fractions, kSZ effect profiles, and galaxy-galaxy lensing
Princeton University（普林斯顿大学）；University of Cambridge（剑桥大学）；Liverpool John Moores University（利物浦约翰摩尔斯大学）；Leiden University（莱顿大学）；University of Zurich（苏黎世大学）
本文通过联合分析eROSITA和HSC-XXL样本的X射线气体质量分数及SDSS/DESI+ACT的kSZ效应轮廓，研究了气体反馈对物质功率谱的抑制效应，发现其抑制幅度在k=1 h Mpc⁻¹时为10±2%，且比主流模拟预测更强。
Cosmological Constraints from Full-Scale Clustering and Galaxy-Galaxy Lensing with DESI DR1
American University（美国大学）；University of Michigan（密歇根大学）；Argonne National Laboratory（阿贡国家实验室）；Smith College（史密斯学院）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
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
Hyper Suprime-Cam Y3 results: photo-$z$ bias calibration with lensing shear ratios and cosmological constraints from cosmic shear
Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Inter University Centre for Astronomy and Astrophysics（大学天文学与天体物理中心）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学 Kavli宇宙物理学与数学研究所（WPI））；Kobayashi-Maskawa Institute for the Origin of Particles and the Universe (KMI), Nagoya University（名古屋大学 Kobayashi-Maskawa粒子宇宙起源研究所（KMI））；Institute for Advanced Research, Nagoya University（名古屋大学高等研究院）；Department of Physics and Astronomy, University of Pennsylvania（宾夕法尼亚大学物理与天文学系）；Department of Physics and Astronomy and PITT PACC, University of Pittsburgh（匹兹堡大学物理与天文学系及PITT PACC）；National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Science（日本国立天文台（NAOJ），国立自然科学研究院）；The Institute of Statistical Mathematics（统计科学研究所）
