X-ray analysis of JWST's first galaxy cluster lens SMACS J0723.3-7327
A. Liu, E. Bulbul, M. E. Ramos-Ceja, J. S. Sanders, V. Ghirardini, Y. E. Bahar, M. Yeung, E. Gatuzz, M. Freyberg, C. Garrel, X. Zhang, A. Merloni, K. Nandra
SMACS~J0723.3-7327 is the first galaxy cluster lens observed by JWST. Based on the ERO data from JWST, several groups have reported the results on strong lensing analysis and mass distribution of this cluster. However, limited by the angular coverage of the JWST data, the strong lensing models only cover the central region. X-ray analysis on the hot ICM is necessary to obtain a more complete constraint on the mass distribution in this very massive cluster. In this work, we aim to perform a comprehensive X-ray analysis of J0723 to obtain accurate ICM hydrostatic mass measurements, using the X-ray data from SRG/eROSITA and Chandra X-ray observatories. By comparing the hydrostatic mass profile with the strong lensing model, we aim to provide the most reliable constraint on the distribution of mass up to R500. Thanks to the eROSITA all-sky survey and Chandra data, which provide high S/N and high angular resolution respectively, we are able to constrain the ICM gas density profile and temperature profile with good accuracy both in the core and to the outskirts. With the density and temperature profiles, we compute the hydrostatic mass profile, which is then projected along the line of sight to compare with the mass distribution obtained from the recent strong lensing analysis based on JWST data. We also deproject the strong lensing mass distribution using the hydrostatic mass profile we obtained in this work. The X-ray results obtained from eROSITA and Chandra agree very well with each other. The hydrostatic mass profiles we measured in this work, both projected and deprojected, are in good agreement with recent strong lensing results based on JWST data, at all radii. We also find that the radial acceleration relation in J0723 is inconsistent with the RAR for spiral galaxies, implying that the latter is not a universal property of gravity across all mass scales.
A Spectroscopic View of the JWST/GTO Strong Lensing Cluster A1489
我们讨论了一个光谱调查的强透镜集群A1489，其中包括195个集群成员的红移以及188个集群成员的中心速度色散。焦散线技术应用于红移测量给出了动力学参数$M_{200} = (1.25~\pm~0.09) \times 10^{15}~M_\odot$、$r_{200} = 1.97~\pm~{0.05}$ Mpc和$r_{200}$内的星团视线速度色散$1150~\pm~{72}~$ km $~$ s $^{-1}$。这些参数与其他具有较大爱因斯坦半径的强透镜系统的参数非常相似。我们使用光谱学和深测光证明，A1489可能是动态活动的，它的四个BCGs有显着不同的休息帧径向速度。像其他大质量强透镜星系团一样，A1489成员的速度色散函数显示出色散$\geq~250~$ km $~$ s $^{-1}$的过量。中心色散还对未来的透镜模型提供了增强的约束。
Lensed stars in galaxy-galaxy strong lensing -- a JWST prediction for the Cosmic Horseshoe
The University of Hong Kong（香港大学）；University of Portsmouth（朴茨茅斯大学）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所（CSIC-UC））；University of Basque Country UPV/EHU（巴斯克大学）；Ikerbasque, Basque Foundation for Science（伊克尔巴斯基，巴斯克科学基金会）；Donostia International Physics Center（圣塞巴斯蒂安国际物理中心）；University of Minnesota（明尼苏达大学）；Universidade Federal do Rio Grande do Sul（南里奥格兰德联邦大学）
TDCOSMO XXIV. First spatially resolved kinematics of the lens galaxy obtained using JWST-NIRSpec to improve time-delay cosmography
Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Center for Astronomy, Space Science and Astrophysics, Independent University, Bangladesh（孟加拉独立大学天文学、空间科学与天体物理中心）；Department of Physics and Astronomy, University of California, Los Angeles（加州大学洛杉矶分校物理与天文系）；Technical University of Munich, TUM School of Natural Sciences, Physics Department（慕尼黑工业大学自然科学院物理系）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Sub-Department of Astrophysics, Department of Physics, University of Oxford（牛津大学物理系天体物理子部门）
JWST lens model for A370: A very low dark matter fraction for a brightest cluster galaxy and lensing properties for the Dragon arc
Tsinghua University（清华大学）；University of Arizona（亚利桑那大学）；Aix Marseille Univ.（艾克斯-马赛大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；Oklahoma State University（俄克拉荷马州立大学）；Arizona State University（亚利桑那州立大学）；University of Pennsylvania（宾夕法尼亚大学）；University of Basque Country UPV/EHU（巴斯克地区大学）；Ikerbasque, Basque Foundation for Science（伊克尔巴斯基克科学基金会）；Donostia International Physics Center（圣塞巴斯蒂安国际物理中心）
An Active Galaxy Cluster Merger at Cosmic Noon Revealed by JWST Weak Lensing and Multiwavelength Probes
Yonsei University（延世大学）；California Institute of Technology（加州理工学院）；University of California Davis（加州大学戴维斯分校）；University of Oxford（牛津大学）；University of California, Los Angeles（加州大学洛杉矶分校）
JWST's PEARLS: 119 multiply imaged galaxies behind MACS0416, lensing properties of caustic crossing galaxies, and the relation between halo mass and number of globular clusters at $z=0.4$
JWST Discovery of Strong Lensing from a Galaxy Cluster at Cosmic Noon: Giant Arcs and a Highly Concentrated Core of XLSSC 122
California Institute of Technology（加州理工学院）；Yonsei University（延世大学）；University of California, Davis（加州大学戴维斯分校）；Korea Astronomy and Space Science Institute（韩国天体宇宙科学研究所）；University of California, Los Angeles（加州大学洛杉矶分校）
Strong LensIng and Cluster Evolution (SLICE) with JWST: Early Results, Lens Models, and High-Redshift Detections
University of Michigan（密歇根大学）；STAR Institute, Quartier Agora - Allée du six Août, 19c B-4000 Liège, Belgium（列日 STAR 研究所）；Durham University（杜伦大学）；Institute for Computational Cosmology, Durham University（杜伦大学计算宇宙学研究所）；Astrophysics Research Centre, University of KwaZulu-Natal（夸祖鲁-纳塔尔大学天体物理研究中心）；School of Mathematics, Statistics & Computer Science, University of KwaZulu-Natal（夸祖鲁-纳塔尔大学数学、统计与计算机科学学院）；Department of Astronomy, University of Washington（华盛顿大学天文学系）；Ecole Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）
TDCOSMO: XX. WFI2033--4723, the First Quadruply-Imaged Quasar Modeled with JWST Imaging
Department of Physics and Astronomy, UCLA（加州大学洛杉矶分校物理与天文系）；Department of Physics and Astronomy, Stony Brook University（纽约州立大学石溪分校物理与天文系）；Department of Astronomy and Astrophysics, University of Chicago（芝加哥大学天文与天体物理系）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Center for Astronomy, Space Science and Astrophysics, Independent University, Bangladesh（孟加拉国独立大学天文学、空间科学与天体物理中心）；Research Center for the Early Universe, Graduate School of Science, The University of Tokyo（东京大学理学研究科早期宇宙研究中心）；IPAC, California Institute of Technology（加州理工学院红外处理分析中心）；Space Telescope Science Institute（太空望远镜科学研究所）
LEGGOS I: The JWST LEGGOS Survey -- LEnsing and Galaxy Growth: Observing Substructures -- Unpacks the Nature of Clumpy Star Formation and Quenching in Gravitationally Lensed Galaxies beyond Cosmic Noon
University of Washington（华盛顿大学）；University of Pittsburgh（匹兹堡大学）；University of Arizona（亚利桑那大学）；Eureka Scientific（尤里卡科学公司）；University of Cincinnati（辛辛那提大学）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）
TDCOSMO. XXVII. JWST-based Lens Models and H$_0$ Measurement of WFI2033, HE0435, and PG1115
University of California, Los Angeles（加州大学洛杉矶分校）；CNRS & Université Montpellier（法国国家科学研究中心与蒙彼利埃大学）；Stony Brook University（纽约州立大学石溪分校）；UC Davis（加州大学戴维斯分校）；University of Geneva（日内瓦大学）；University of Chicago（芝加哥大学）；Independent University, Bangladesh（孟加拉独立大学）；The University of Tokyo（东京大学）
Mapping dark matter in the Bullet Cluster using JWST imaging and spectroscopy
Department of Physics and Astronomy, University of California Davis（加州大学戴维斯分校物理与天文学系）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory - Astrophysics Group, University of Cambridge（剑桥大学卡文迪许实验室天体物理组）；National Research Council of Canada, Herzberg Astronomy & Astrophysics Research Centre（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究中心）；Department of Physics and Astronomy, York University（约克大学物理与天文学系）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学大卫·A·邓纳普天文学与天体物理学系）
The free-streaming length of dark matter from JWST observations of 28 strong gravitational lenses
University of Chicago（芝加哥大学）；University of California, Merced（加州大学默塞德分校）；University of California, Los Angeles（加州大学洛杉矶分校）；University of California, Irvine（加州大学尔湾分校）；Universidad Andres Bello（安德斯·贝略大学）；California Polytechnic State University（加州州立理工大学）；Carnegie Institution for Science（卡内基科学机构）；Stony Brook University（石溪大学）；California Institute of Technology（加州理工学院）；University of Southampton（南安普顿大学）
Hedorah, the first yellow supergiant Kaiju star candidate at $z=3.7$ revealed by JWST behind AS1063
Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）；School of Physics and Astronomy, University of Minnesota（明尼苏达大学物理与天文学院）；STAR Institute（STAR研究所）；Université Claude Bernard Lyon 1（里昂第一大学）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；Department of Physics and Astronomy, University of Pennsylvania（宾夕法尼亚大学物理与天文学系）
JWST lensed quasar dark matter survey V: Hints of self-interacting dark matter from 29 quadruply imaged quasars
University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙学物理研究所）；University of California, Merced（加州大学默塞德分校）；Perimeter Institute for Theoretical Physics（理论物理前沿研究所）；Carnegie Observatories（卡内基观测站）；University of California, Los Angeles（加州大学洛杉矶分校）；University of California, Irvine（加州大学尔湾分校）；Universidad Andres Bello（安德烈斯贝略大学）；Millennium Institute of Astrophysics, Chile（智利天体物理千年研究所）；California Polytechnic State University（加州州立理工大学）
SN 2022riv in RX J2129: Discovery, Spectroscopic Classification, and Microlensing of a Strongly Lensed Type Ia Supernova from JWST and HST Observations
University of Minnesota（明尼苏达大学）；Oklahoma State University（俄克拉荷马州立大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Chiba University（千叶大学）；Instituto de Física de Cantabria（坎塔布里亚物理研究所）
TDCOSMO XXX: Spatially resolved kinematics of the deflectors in time-delay lens systems B1608+656 and SDSSJ1206+4332 from JWST-NIRSpec observation
University of California, Los Angeles（加州大学洛杉矶分校）；University of Chicago（芝加哥大学）；Independent University, Bangladesh（孟加拉独立大学）；University of Oxford（牛津大学）；Technical University of Munich（慕尼黑工业大学）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）
Two lensed star candidates at $z\simeq4.8$ behind the galaxy cluster MACS J0647.7+7015
我们报道了在最近的多波段詹姆斯·韦伯太空望远镜（JWST）近红外摄像机观测中，在星系团MACS J0647.7+7015后面发现了两个极度放大的透镜状恒星候选者。候选者出现在先前已知的、横跨临界曲线的$z_{phot}\simeq4.8$脱落巨弧中。候选者位于预期的临界曲线位置附近，但在另一边缺乏清晰的反像，这表明它们可能是正在经历焦散交叉的恒星。我们提出了修订后的透镜模型的集群，包括多成像星系新发现的JWST数据，并使用它们来估计至少$\gtrsim90$和$\gtrsim50$在两个候选人的位置，分别的背景宏观放大率。有了这些值，我们期望两个候选恒星的$10^4-10^5$的有效的、焦散性交叉放大率。这两个候选人的光谱能量分布（SED）匹配以及光谱的B-型恒星的最佳拟合表面温度分别为$\sim10,000$ K和$\sim12,000$ K，我们表明，这样的恒星质量$\gtrsim20$ M $_{\odot}$和$\gtrsim50$ M $_{\odot}$，分别可以成为足够的放大被观察。我们简要地讨论了其他的解释，并得出结论，这些可能是透镜星，但也承认，放大较小的候选人可能是或居住在星团。这些恒星候选者构成了继$z_{phot}\simeq6.2$的埃伦德尔之后，迄今为止第二高红移的例子，进一步建立了利用JWST研究极度放大恒星到高红移的潜力。包括近红外光谱观测在内的计划…
Fast Lensing And Sub-minute High-accuracy photometry (FLASH) with JWST: Pipeline and Primordial Black Hole Microlensing Constraints from M31
University of Hawai‘i at Mānoa（夏威夷大学马诺阿分校）；E.O. Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Institute for Astronomy, University of Hawai‘i at Mānoa（夏威夷大学马诺阿分校天文研究所）
