We present an analysis of the role of feedback in shaping the neutral hydrogen (HI) content of simulated disc galaxies. For our analysis, we have used two realisations of two separate Milky Way-like (~L*) discs - one employing a conservative feedback scheme (MUGS), the other significantly more energetic (MaGICC). To quantify the impact of these schemes, we generate zeroth moment (surface density) maps of the inferred HI distribution; construct power spectra associated with the underlying structure of the simulated cold ISM, in addition to their radial surface density and velocity dispersion profiles. Our results are compared with a parallel, self-consistent, analysis of empirical data from THINGS (The HI Nearby Galaxy Survey). Single power-law fits (P~k^gamma) to the power spectra of the stronger-feedback (MaGICC) runs (over spatial scales corresponding to 0.5 kpc to 20 kpc) result in slopes consistent with those seen in the THINGS sample (gamma = -2.5). The weaker-feedback (MUGS) runs exhibit shallower power law slopes (gamma = -1.2). The power spectra of the MaGICC simulations are more consistent though with a two-component fit, with a flatter distribution of power on larger scales (i.e., gamma = -1.4 for scales in excess of 2 kpc) and a steeper slope on scales below 1 kpc (gamma = -5), qualitatively consistent with empirical claims, as well as our earlier work on dwarf discs. The radial HI surface density profiles of the MaGICC discs show a clear exponential behaviour, while those of the MUGS suite are essentially flat; both behaviours are encountered in nature, although the THINGS sample is more consistent with our stronger (MaGICC) feedback runs.
Interplay between Escaping Cosmic Rays and Interstellar Medium: Driving of Galactic Winds and Shaping the Local Proton Spectrum
Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Department of Physics, Graduate School of Science, Nagoya University（名古屋大学理学研究科物理学系）
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）
Cosmological simulations of the same spiral galaxy: satellite properties, the role of baryonic physics and star formation history in shaping dark matter cores/cusps
The mass-dependent interplay of active galacitc nuclei and supernova feedback in shaping the $L_{\rm X}$--$T$ relation of early-type galaxies
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）；Center for Astronomy and Astrophysics and Department of Physics, Fudan University（复旦大学天文与天体物理中心及物理系）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
The Impact of Star Formation and Feedback Recipes on the Stellar Mass and Interstellar Medium of High-Redshift Galaxies
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物理研究所）；University of Oxford（牛津大学）；Lund University（隆德大学）；Yonsei University（延世大学）
A Spatially Resolved HI Survey of Seyfert Galaxies: the Role of AGN Feedback in Shaping Atomic Gas Reservoirs
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences (UCAS)（中国科学院大学天文与空间科学学院）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学天文与空间科学学院前沿科学中心）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）
AGN Feedback: The impact of galactic-scale radio jets on the interstellar medium in starbursting obscured AGN
INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano（意大利国家天体物理研究所空间天体物理学与宇宙学米兰分院）；Associated Universities, Inc.（联合大学公司）；William H. Miller III Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学威廉·H·米勒三世物理与天文系）；MIT Haystack Observatory（麻省理工学院海斯塔克天文台）
Surveying the Whirlpool at Arcseconds with NOEMA (SWAN). IV. Extent of active galactic nucleus feedback on the interstellar medium
Universität Bonn（波恩大学）；Observatorio Astronómico Nacional (IGN)（国家天文台（西班牙地理与测绘研究所））；The Ohio State University（俄亥俄州立大学）；Center for Cosmology and Astro-Particle Physics, Ohio State University（俄亥俄州立大学宇宙学与天体粒子物理中心）；National Astronomical Observatory of Japan（日本国立天文台）；Max Planck Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；University of Arkansas（阿肯色大学）
Three-phase Interstellar medium in Galaxies Resolving Evolution with Star formation and Supernova feedback (TIGRESS): Algorithms, Fiducial model, and Convergence
Rhea-RT: Dynamical impact of Central Molecular Zone conditions on the properties of the interstellar medium and stellar feedback coupling
EPFL（洛桑联邦理工学院）；ENS de Lyon, Université Lyon 1, CNRS, CRAL（里昂高等师范学校，里昂第一大学，法国国家科学研究中心，天体物理与宇宙学研究中心）；Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik（海德堡大学，天文中心，理论天体物理研究所）；Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen（海德堡大学，跨学科计算科学中心）
Massive star feedback in clusters: variation of the FUV interstellar radiation field in time and space
利用三维辐射流体力学（RHD）模型研究了34 M $_\odot$恒星在$10^4$ M $_\odot$湍流云中的辐射反馈。我们使用蒙特卡罗辐射转移精确计算光电离平衡和辐射压力，与多个原子物种和硅酸盐尘埃颗粒。我们包括漫射辐射场，灰尘吸收/再发射，和散射。云被有效地分散，75%的质量在430万年（110万年$t_{ff}$）内离开$^3$网格（32.3pc）。这与我们以前发表的$10^3$ M $_\odot$云中160万年（0.74 $t_{ff}$）内的所有质量进行了比较。最多有20%的质量是电离的，而在较低质量的模型中是40%，尽管两者的电离体积分数都是80%，这意味着较高质量的云对反馈更具弹性。总的Jeans不稳定质量线性增加到1500 M $_\odot$，然后在200万年后趋于稳定，对应于15%的核心形成效率。我们还测量了远紫外（FUV）辐射场的时间变化，$G_0$，撞击其他集群成员，第一次考虑到这是如何在动态集群环境中与干预不透明源和恒星运动的变化。在最初的0.5百万年里，许多天体仍然被遮蔽，而大质量恒星被嵌入其中，之后$G_0$以数量级增加。后来的气体运动引起了类似的瞬间下降，并在恢复之前持续了$\sim$ 1百万年。这种高度变化的紫外光场将影响大质量恒星附近原行星盘的光蒸发。
The fate of the interstellar medium in early-type galaxies. IV. The impact of stellar feedback, mergers, and black holes on the cold ISM in simulated galaxies
The Interstellar Medium and star formation on kpc size scales
通过重新模拟一个区域的全球光盘模拟在更高的分辨率，我们解决和研究的分子云的性质，从几个100的M $_{\odot}$到$10^6$ M $_{\odot}$的质量范围。我们的论文的目的是双重的，i）比较ISM和GMC在更高的分辨率相比，以前的全球模拟，和ii）调查较小的云和特性，如GMC的内部属性，不能解决在银河系模拟。我们确认了在以前的银河系模拟中看到的云属性的鲁棒性，这些属性扩展到较低质量的云，虽然我们警告说，速度分散可能无法正确地测量在分辨率差的云。我们发现，云和ISM的属性只有弱依赖于本地恒星反馈的细节，虽然恒星反馈是重要的，以产生现实的恒星形成率和协议的施密特-肯尼库特关系。我们研究了$10^4-10^5$粒子分解的GMCs的内部性质。云是高度结构化的，但我们发现云有一个速度色散半径的关系，总体上同意与拉森关系。GMC显示了恒星形成的多个事件的证据，与之前的反馈事件相对应的洞和密集的区域可能即将形成恒星。我们的模拟显示了明显的长纤维，主要见于臂间区域和壳。
