Two of the dominant channels for galaxy mass assembly are cold flows (cold gas supplied via the filaments of the cosmic web) and mergers. How these processes combine in a cosmological setting, at both low and high redshift, to produce the whole zoo of galaxies we observe is largely unknown. Indeed there is still much to understand about the detailed physics of each process in isolation. While these formation channels have been studied using hydrodynamical simulations, here we study their impact on gas properties and star formation (SF) with some of the first simulations that capture the multiphase, cloudy nature of the interstellar medium (ISM), by virtue of their high spatial resolution (and corresponding low temperature threshold). In this regime, we examine the competition between cold flows and a supernovae(SNe)-driven outflow in a very high-redshift galaxy (z {\approx} 9) and study the evolution of equal-mass galaxy mergers at low and high redshift, focusing on the induced SF. We find that SNe-driven outflows cannot reduce the cold accretion at z {\approx} 9 and that SF is actually enhanced due to the ensuing metal enrichment. We demonstrate how several recent observational results on galaxy populations (e.g. enhanced HCN/CO ratios in ULIRGs, a separate Kennicutt Schmidt (KS) sequence for starbursts and the population of compact early type galaxies (ETGs) at high redshift) can be explained with mechanisms captured in galaxy merger simulations, provided that the multiphase nature of the ISM is resolved.
Observational Evidence of Velocity Anisotropy Assembly Bias in Galaxy Clusters
CONICET. Instituto de Astronomía Teórica y Experimental (IATE)（阿根廷国家科学研究委员会理论与实验天体物理研究所）；Universidad Nacional de Córdoba (UNC). Observatorio Astronómico de Córdoba (OAC)（科尔多瓦国立大学科尔多瓦天文台）；INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；IFPU Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Centre for Particle Cosmology, University of Pennsylvania（宾夕法尼亚大学粒子宇宙学中心）；Departamento de Física, Universidad Técnica Federico Santa María（智利费德里科·Santa María理工大学物理系）
Luminosity-Dependent Assembly Bias of Central Galaxies from Weak Lensing and Clustering
Shanghai Jiao Tong University（上海交通大学）；Graduate School of Science, Nagoya University（名古屋大学理学研究科）；Kobayashi-Maskawa Institute for the Origin of Particles and the Universe (KMI), Nagoya University（名古屋大学小林-益川粒子宇宙起源研究所）；Institute for Advanced Research, Nagoya University（名古屋大学高等研究院）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学理化学研究所 Kavli 宇宙粒子物理学研究所）；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）；Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理研究所）
Halo assembly bias in the early Universe: a clustering probe of the origin of the Little Red Dots
Peking University（北京大学）；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）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院科维理天体物理与空间研究）
Baryonic assembly bias in X-ray-selected galaxy groups and clusters: insights from the Magneticum simulation
European Southern Observatory（欧洲南方天文台）；Excellence Cluster ORIGINS（卓越集群ORIGINS）；Ludwig-Maximilians-Universität München（慕尼黑大学）；University of São Paulo（圣保罗大学）；INAF – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；IFPU – Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；ICSC - Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing（高性能计算、大数据和量子计算国家研究中心）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
Connecting clustering and the cosmic web:Observational constraints on secondary halo bias
CONICET. Instituto de Astronomía Teórica y Experimental (IATE)（阿根廷国家科学研究委员会理论天体物理学研究所）；Universidad Nacional de Córdoba (UNC). Observatorio Astronómico de Córdoba (OAC)（科尔多瓦国立大学科尔多瓦天文台）；Departamento de Física, Universidad Técnica Federico Santa María（圣马利亚技术大学物理系）
Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies in the Local Universe I. - The Effect of the Group Environment on Star Formation in Spiral Galaxies
Spatially resolved metallicity and ionization in the merging system Gz9p3 at z=9.3
Stockholm University（斯德哥尔摩大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家研究委员会-国家航空技术研究所）；Space Telescope Science Institute (STScI)（太空望远镜科学研究所）；University of Copenhagen（哥本哈根大学）；UK Astronomy Technology Centre, Royal Observatory Edinburgh（英国天文学技术中心，爱丁堡皇家天文台）
The Pandora project. II: how non-thermal physics drives bursty star formation and temperate mass-loaded outflows in dwarf galaxies
Stanford University（斯坦福大学）；University of Cambridge（剑桥大学）；European Southern Observatory（欧洲南方天文台）；SLAC National Accelerator Laboratory（史拉格国家加速器实验室）；The University of Chicago（芝加哥大学）；EPFL（洛桑联邦理工学院）；University of Oxford（牛津大学）；Sorbonne Université（索邦大学）；Univ Lyon1（里昂第一大学）；University of South Carolina（南卡罗来纳大学）
The MandelZoom project II: the impact of stellar feedback on black hole accretion through an $α$-disc in dwarf galaxies with a resolved interstellar medium
Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文与数学系天体物理研究中心）；St Catharine’s College, University of Cambridge（剑桥大学圣凯瑟琳学院）
Direct detection of cool molecular gas in a star-forming galaxy at $z=7.31$
Leiden University（莱顿大学）；Academia Sinica（中央研究院）；Universität zu Köln（科隆大学）；Liverpool John Moores University（利物浦约翰摩尔斯大学）；Ghent University（根特大学）；Universidad Diego Portales（迭戈帕托莱斯大学）
