The role of galactic wind recycling represents one of the largest unknowns in galaxy evolution, as any contribution of recycling to galaxy growth is largely degenerate with the inflow rates of first-time infalling material, and the rates with which outflowing gas and metals are driven from galaxies. We present measurements of the efficiency of wind recycling from the EAGLE cosmological simulation project, leveraging the statistical power of large-volume simulations that reproduce a realistic galaxy population. We study wind recycling at the halo scale, i.e. gas that has been ejected beyond the halo virial radius, and at the galaxy scale, i.e. gas that has been ejected from the ISM to at least $\approx 10 \, \%$ of the virial radius (thus excluding smaller-scale galactic fountains). Galaxy-scale wind recycling is generally inefficient, with a characteristic return timescale that is comparable or longer than a Hubble time, and with an efficiency that clearly peaks at the characteristic halo mass of $M_{200} = 10^{12} \, \mathrm{M_\odot}$. Correspondingly, the majority of gas being accreted onto galaxies in EAGLE is infalling for the first time. At the halo scale, the efficiency of recycling onto haloes differs by orders of magnitude from values assumed by semi-analytic galaxy formation models. Differences in the efficiency of wind recycling with other hydrodynamical simulations are currently difficult to assess, but are likely smaller. We are able to show that the fractional contribution of wind recycling to galaxy growth is smaller in EAGLE than in some other simulations. We find that cumulative first-time gas accretion rates at the virial radius are reduced relative to the expectation from dark matter accretion for haloes with mass, $M_{200} < 10^{12} \, \mathrm{M_\odot}$, indicating efficient preventative feedback on halo scales.
Satellite Metallicity Enhancement I: Suppressed Star Formation, Stellar Mass Loss, and Enriched Inflow of DESI and EAGLE Galaxies around Massive Clusters
State Key Laboratory of Dark Matter Physics & Tsung-Dao Lee Institute, Shanghai Jiao Tong University（暗物质物理国家重点实验室暨李政道研究所，上海交通大学）；Department of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University（上海交大物理与天文学院天文学系）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Department of Physics, Boston University（波士顿大学物理系）；Department of Physics & Astronomy, University College London（伦敦大学学院物理与天文系）；Instituto de Física, Universidad Nacional Autónoma de México（墨西哥国立自治大学物理研究所）
A comparison of observed and simulated absorption from HI, CIV, and SiIV around $z\approx2$ star-forming galaxies suggests redshift-space distortions are due to inflows
我们研究HI和金属线吸收$z\approx2$恒星形成星系周围的凯克重子结构调查模拟光谱的EAGLE宇宙学，流体动力学模拟产生的数据进行比较分析。我们从模拟中提取视线，并比较HI，CIV和SiIV的吸收特性模拟和观察星系使用像素光学深度。我们模拟的分辨率，像素大小，和观测的信噪比，以及分布的碰撞参量和星系红移误差。我们发现EAGLE参考模型与观测结果非常吻合。特别是，模拟再现高金属线的光学深度发现在小银河系的距离，光学深度增强到碰撞参量的2个适当的Mpc，和突出的红移空间的扭曲，我们发现是由于特殊的速度，而不是红移误差。晕质量$\sim10^{12.0}$ M $_\odot$的一致性最好，观测和模拟的恒星质量也最接近。我们研究了星系周围的中值离子质量加权径向气体速度，发现大部分气体都在下落，下落速度取决于晕而不是恒星质量。从这一点，我们得出结论，观察到的红移空间的扭曲主要是由流入，而不是流出。
Aligned and misaligned metallicity gradients in young stars and star-forming regions in the EAGLE discs
Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Instituto de Astrofísica, Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学天体物理研究所）；Centro de Astro-Ingeniería, Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学天文工程学院）
The Cosmic Baryon Cycle in IllustrisTNG: flows of mass, energy, and metals
Tel Aviv University（特拉维夫大学）；Columbia University（哥伦比亚大学）；Flatiron Institute（平顿研究所）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）
Widespread Inflows Reveal Baryonic Cycling in Star-forming and Quiescent Galaxies
Chinese Academy of Sciences（中国科学院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Indian Institute of Astrophysics (IIA)（印度天体物理研究所）；Fudan University（复旦大学）；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）；Department of Physics, Fudan University（复旦大学物理系）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；International Centre for Radio Astronomy Research, University of Western Australia（西澳大利亚大学国际无线电天文研究中心）；University of Western Australia（西澳大利亚大学）
Diverse Metallicities in Protoclusters at $z \sim 3.4$ detected by Deep Learning
The University of Tokyo（东京大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心 (DAWN)）；Technical University of Denmark（丹麦技术大学）；University of Hyogo（兵库大学）；Tohoku University（东北大学）；Kwansei Gakuin University（关西学院大学）；Carnegie Institution for Science（卡内基科学机构）；National Astronomical Observatory of Japan（日本国立天文台）
