Observational studies have established a remarkably tight power-law relationship between the H I masses and sizes of late-type galaxies, known as the H I mass-size relation. This relation has been shown to persist across various models of a galaxy's H I surface density profile. Using the Simba cosmological simulations, we investigate the robustness of this relation under different feedback prescriptions, including cases where specific feedback mechanisms are absent. While the global properties of galaxies are significantly affected by changes in feedback, the H I mass-size relation remains intact. Moreover, its parameters consistently align with the best available empirical measurements. We analyze the H I mass distributions of galaxies and demonstrate that, regardless of the feedback scenario, galaxies within a given H I mass bin exhibit outer H I radial profiles well approximated by an exponential function. Furthermore, the exponential decline rate remains remarkably similar across different physical prescriptions. We attribute the persistence of the H I mass-size relation to this inherent self-similarity in the H I mass distributions.
Using the Simba cosmological simulations to measure the planar relation between stellar specific angular momentum, mass and effective surface brightness
Investigating the residuals in the $M_\bullet-M_*$ relation using the SIMBA cosmological simulation
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；the University of Chinese Academy of Sciences（中国科学院大学）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Department of Physics, University of Connecticut（康涅狄格大学物理系）
Forged by Feedback: Stellar Properties of Brightest Group Galaxies in Cosmological Simulations
University of Victoria（维多利亚大学）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；Indian Institute of Science（印度科学学院）；Aalto University（阿尔托大学）；University of Helsinki（赫尔辛基大学）；University of the Western Cape（西开普大学）
Analysis of synthetic OVI absorption associated with galaxy groups in SIMBA and TNG50 simulations
School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Universität Heidelberg, Zentrum für Astronomie, ITA（海德堡大学天文学中心ITA）；Institute for Astronomy, University of Edinburgh, Royal Observatory（爱丁堡大学皇家天文台天体物理研究所）；Department of Physics and Astronomy, University of the Western Cape（西开普大学物理与天文学系）
CASCO: Cosmological and AStrophysical parameters from Cosmological simulations and Observations -- I. Constraining physical processes in local star-forming galaxies
The CAMELS project: Expanding the galaxy formation model space with new ASTRID and 28-parameter TNG and SIMBA suites
Harvard-Smithsonian Center for Astrophysics（哈佛-史密松天体物理中心）；Carnegie Mellon University（卡内基梅隆大学）；Flatiron Institute（弗莱提荣研究所）；Columbia University（哥伦比亚大学）；University of Connecticut（康涅狄格大学）；Princeton University（普林斯顿大学）；University of California, Riverside（加州大学河滨分校）
Simba: The average properties of the circumgalactic medium of $2 \leq z \leq 3$ quasars are determined primarily by stellar feedback
利用Simba宇宙流体动力学模拟软件包研究了反馈对$2 \leq z \leq 3$类星体周围环星系介质和星系际介质的影响。我们发现辛巴类星体是吸积速度最快的黑洞，并表明它们在热光度和相关强度上与真正的类星体很好地匹配。我们提取莱曼α（Ly-a）吸收光谱通过在不同的横向距离（10千秒差距$\lesssim b \lesssim$ 10百万秒差距）周围的类星体，并比较观察到的平均Ly-a吸收曲线。观测结果被很好地再现，除了在100 kpc的前景类星体，辛巴过度产生吸收;这可能会通过包括类星体本身的电离来减轻。通过比较不同的反馈模块激活的运行，我们发现，（机械）AGN反馈对周围的CGM几乎没有影响，即使在这些最高亮度的黑洞，而恒星反馈有显着的影响。通过进一步研究CGM气体的热力学和运动学性质，我们发现恒星反馈而不是活动星系核反馈是决定$z\sim 2-3$类星体周围CGM平均性质的主要物理驱动因素。我们还比较了我们的结果与以前的作品，并发现辛巴预测更多的吸收在100千秒差距内比尼克斯和Illustris模拟，表明Ly-a吸收曲线可以是一个强大的约束模拟。VLT-MUSE等工具和即将进行的调查（例如，WEAVE和DESI）承诺进一步改进此类约束。
Populating Galaxies Into Halos Via Machine Learning on the Simba Simulation
School of Mathematics and Physics, University of Queensland（昆士兰大学数学与物理学院）；Institute for Astronomy, Royal Observatory, Edinburgh（爱丁堡皇家天文台天体物理研究所）；School of Physical Sciences, National Institute of Science Education and Research, HBNI（印度国家科学教育与研究中心物理科学学院，HBNI）；Departamento de Física Teórica, Universidad Autónoma de Madrid（马德里自治大学理论物理系）；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高级研究中心）；Department of Physics and Astronomy, University of the Western Cape（西开普大学物理与天文学系）
What's Missing in AGN Feedback? Lessons learnt from Magneticum, IllustrisTNG and Simba
European Southern Observatory（欧洲南方天文台）；Excellence Cluster ORIGINS（ORIGINS卓越集群）；Universitäts-Sternwarte, Fakultät für Physik, LMU（慕尼黑大学天文台，物理学院）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理学研究所）
Introducing RAFIKI: Refining AGN Feedback in Kinetic Implementations
School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Institute for Astronomy, Royal Observatory, University of Edinburgh（爱丁堡大学皇家天文台天体物理研究所）；Department of Physics and Astronomy, University of the Western Cape（西开普大学物理与天文学系）；Stellenbosch Institute for Advanced Studies（斯特伦博斯高等研究院）；Department of Physics and Astronomy, University of Victoria（维多利亚大学物理与天文学系）；Leverhulme Visiting Professor（莱弗休姆访问教授）；Centre for Space Research, North-West University（西北大学太空研究中心）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）
Investigating the [C$\,{\rm \scriptsize II}$]-to-H$\,{\rm \scriptsize I}$ conversion factor and the H$\,{\rm \scriptsize I}$ gas budget of galaxies at $z\approx 6$ with hydrodynamical simulations
The kinetic Sunyaev Zeldovich effect as a benchmark for AGN feedback models in hydrodynamical simulations: insights from DESI + ACT
Institute of Astronomy, University of Cambridge（剑桥大学天体物理研究所）；Kavli Institute for Cosmology (KICC), University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学天体物理研究所）；Institute for Astronomy, Royal Observatory, Univ. of Edinburgh（爱丁堡大学皇家天文台天体物理研究所）；University of the Western Cape（西开普大学）；South African Astronomical Observatories（南非天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Lorentz Institute for Theoretical Physics, Leiden University（莱顿大学洛伦兹理论物理研究所）
The Structural Abundance Crisis of Massive Galaxies in Current Cosmological Simulations
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；International Centre for Radio Astronomy Research, University of Western Australia（西澳大利亚大学国际射电天文学研究中心）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；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）
