Intracluster globular clusters as tracers of the mass assembly of the Hydra I galaxy cluster
European Southern Observatory（欧洲南方天文台）；Universitätssternwarte der Ludwig-Maximilians Universität（路德维希-马克西米利安大学大学天文台）；INAF – Astronomical Observatory of Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；INAF – Astronomical Observatory of Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Gran Sasso Science Institute（格兰萨索科学研究所）
Felipe S. Lohmann, Magda Arnaboldi, Michael Hilker, Andreas Burkert, Marilena Spavone, Ortwin Gerhard, Marina Rejkuba, Marco Mirabile, Michele Cantiello, Enrichetta Iodice
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Accepted for publication in A&A. 19 pages, 20 figures
In galaxy clusters, hierarchical assembly predicts the formation of stellar substructures and intracluster light (ICL), a diffuse stellar component tracing the global cluster potential. Because these features are extremely faint, alternative tracers such as globular clusters (GCs) provide a powerful tool to study cluster assembly. We use deep VLT/FORS $V$- and $I$-band imaging to investigate the GC population in the nearby Hydra I galaxy cluster ($\sim 45.7$ Mpc). GC candidates were selected from the $VI$ colour-magnitude diagram and divided into blue and red subpopulations. We find a clear spatial dichotomy: red GCs are concentrated around the massive central galaxies NGC 3311 and NGC 3309, while blue GCs are more extended and offset from the centre, coinciding with a secondary peak of X-ray-emitting gas. In the central regions, GC spatial distributions further depend on stellar population properties: young metal-rich GCs are more extended and may be linked to ram-pressure stripping, whereas old metal-poor GCs are more centrally concentrated, possibly originating from disrupted dwarf galaxies. Comparing the GC number density profiles to the surface brightness profile of NGC 3311, we find that the red GCs closely follow the galaxy light, while the blue population significantly deviates from it and traces the global gravitational potential of the cluster. This is also reflected in the specific frequency of blue GCs, which is approximately $\sim 5\times$ higher in the ICL-dominated outskirts than in the inner regions dominated by red GCs. Finally, we present a novel method to constrain the evolution of the galaxy luminosity function of the cluster using GC specific frequencies and colour distributions, yielding a past faint-end slope of $α=-1.81^{+0.16}_{-0.16}$ compared to $α=-1.41^{+0.08}_{-0.05}$ today, consistent with high-redshift observations and cosmological simulations.
Intracluster light as a dark matter tracer: how their spatial and kinematic relationship is shaped by satellite demographics
University of Nottingham（诺丁汉大学）；École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；Universidad Autónoma de Madrid（马德里自治大学）；Royal Observatory, Edinburgh（爱丁堡皇家天文台）
Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution?
我们利用暗能量巡天（DES）第一年数据中发现的528个$0.2\leq z \leq 0.35$星系团的样本，探讨了团内漫射光（包括中央星系）和星系团（重子和暗）物质分布之间的关系。漫射光的表面亮度在较大的半径上表现出对团簇总质量的依赖性，并且在按团簇半径缩放后表现出具有普遍径向依赖性的自相似性。我们还比较了通过弱透镜测量的集群（重子和暗）物质分布的漫射光径向配置文件，并发现它们是可比的。IllustrisTNG星系形成模拟，TNG 300，提供了进一步的洞察扩散恒星质量和集群物质分布之间的联系-扩散恒星成分的模拟径向轮廓没有与总集群物质含量类似的斜率，虽然集群卫星星系的斜率。无论径向趋势如何，扩散恒星质量的数量与模拟中的星系团总质量具有低散射标度关系，优于星系团卫星星系的总恒星质量。我们的结论是，目前还没有一致的证据，是否漫射光是一个忠实的径向示踪剂的集群物质分布。然而，观测和模拟结果都表明，漫射光是星团总质量的一个很好的指标。
Tracing Dark Matter in the Central Regions of Galaxy Clusters Using Galaxies, Gas, and Intracluster Light in TNG300: Connections to Cluster Dynamical State
Extragalactic planetary nebulae -- tracers of kinematics and stellar populations out to 100 Mpc
University of Turku（图尔库大学）；European Southern Observatory（欧洲南方天文台）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理研究所）；University of Hertfordshire（赫特福德大学）；University of Oxford（牛津大学）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；Universität Potsdam（波茨坦大学）；Ludwig-Maximilians-Universität München（慕尼黑大学）
The Open Cluster Chemical Abundances and Mapping Survey: V. Chemical Abundances of CTIO/Hydra Clusters using The Cannon
疏散星团是银河系演化的重要化学和年龄示踪物。虽然疏散星团对星系演化提供了重要的限制，但由于不同研究在测量丰度方面的差异，它们的使用受到了限制。我们使用Cannon分析了58个疏散星团中巨星的中等分辨率（R~19，000）CTIO/Hydra光谱，确定了[Fe/H]、[Mg/Fe]、[Si/Fe]、[Al/Fe]和[O/Fe]。这项工作增加了一个额外的55个主要是南半球的疏散星团校准到SDSS/APOGEE DR 16金属丰度系统。这种统一的分析相比，以前的研究[Fe/H]测量的23个集群，我们提出的光谱金属丰度为35疏散星团的第一次。
Intracluster Light as a Probe for Dark Matter: Exploring Self-interacting Dark Matter and Cold Dark Matter with C-EAGLE Sims
Korea Astronomy and Space Science Institute (KASI)（韩国天文学与空间科学研究所）；Quantum Universe Center, Korea Institute for Advanced Study（量子宇宙中心，韩国高等研究院）；School of Physics, The University of Sydney（悉尼大学物理学院）；ARC Centre of Excellence for Dark Matter Particle Physics（暗物质粒子物理卓越研究中心）；Departamento de Física Teórica, Facultad de Ciencias M-8, Universidad Autónoma de Madrid（马德里自治大学理学院M-8理论物理系）；Natural Science Research Institute (NSRI), University of Seoul（首尔大学自然科学研究所）；School of Physics, Korea Institute for Advanced Study（韩国高等研究院物理学院）；School of Physics and Astronomy, University of Nottingham（诺丁汉大学物理与天文学院）；Center for Advanced Computation, Korea Institute for Advanced Study（韩国高等研究院先进计算中心）；University of Science and Technology (UST)（科学技术院）
Intracluster light and dark matter halo shapes reflect common assembly, not mutual coupling: shape correspondence in CDM but not SIDM
School of Physics & Astronomy, University of Nottingham（诺丁汉大学物理与天文学院）；Universidad Autónoma de Madrid（马德里自治大学）；Centro de Investigación Avanzada en Física Fundamental (CIAFF), Facultad de Ciencias, Universidad Autónoma de Madrid（马德里自治大学理学院基础物理前沿研究中心）；Institute for Astronomy, Royal Observatory, Edinburgh（爱丁堡皇家天文台天体物理研究所）；Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院天体物理实验室）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（加泰罗尼亚高等研究理事会））
The SRG/eROSITA All-Sky Survey: A comprehensive X-ray analysis of the Hydra I galaxy cluster
Universität Bonn（波恩大学）；Università degli studi di Roma ‘Tor Vergata’（罗马托维尔加塔大学）；INFN, Sezione di Roma 2（意大利国家核物理研究所罗马第二分部）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Universität Erlangen-Nürnberg（埃尔朗根-纽伦堡大学）
Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra I cluster III. Untangling UDG 32 from the stripped filaments of NGC 3314A with multi-wavelength data
A Consistent Comparison of Intracluster Light Assembly in Simulations I. Redshift Evolution and Progenitor Galaxies
University of Nottingham（诺丁汉大学）；École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；Universidad Autónoma de Madrid（马德里自治大学）；Royal Observatory, Edinburgh（爱丁堡皇家天文台）
A model for the ongoing subcluster interaction in Centaurus
European Southern Observatory（欧洲南方天文台）；Universitätssternwarte der Ludwig-Maximilians Universität（路德维希-马克西米利安大学大学天文台）；INAF – Astronomical Observatory of Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；Departamento de Astronomía, Universidad de Concepción（康塞普西翁大学天文学系）；INAF – Astronomical Observatory of Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Gran Sasso Science Institute（格兰萨索科学研究所）
Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra-I cluster IV. A study of the Globular Cluster population in four UDGs
INAF Osservatorio Astr. d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；European Southern Observatory（欧洲南方天文台）；Gran Sasso Science Institute（格兰萨索科学研究所）；INAF – Astronomical Observatory of Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Centre for Astrophysics and Supercomputing, Swinburne University（斯威本大学天体物理学与超级计算中心）；Finnish Centre for Astronomy with ESO, (FINCA), University of Turku（图尔库大学芬兰ESO天文学中心）；Tuorla Observatory, Department of Physics and Astronomy, University of Turku（图尔库大学物理与天文学系图奥拉天文台）；Turku Collegium for Science, Medicine and Technology（图尔库科学技术学院）
Wiggling Through the ICM: Multi-Resolution Radio Imaging of a Tailed Radio Galaxy in MACS J1354.6+7715
Durham University（杜伦大学）；Indian Institute of Science Education and Research Mohali（印度科学教育研究所莫哈利分校）；Institute for Computational Cosmology, Department of Physics, Durham University（杜伦大学物理学院计算宇宙学研究所）；National Centre for Radio Astrophysics, TIFR（印度天文物理国家射电中心，塔塔基础研究院）；Centre for Space Research, North-West University（西北大学空间研究中心）
