Characterizing mass, momentum, energy and metal outflow rates of multi-phase galactic winds in the FIRE-2 cosmological simulations
Viraj Pandya, Drummond B. Fielding, Daniel Anglés-Alcázar, Rachel S. Somerville, Greg L. Bryan, Christopher C. Hayward, Jonathan Stern, Chang-Goo Kim, Eliot Qua… 展开作者
Viraj Pandya, Drummond B. Fielding, Daniel Anglés-Alcázar, Rachel S. Somerville, Greg L. Bryan, Christopher C. Hayward, Jonathan Stern, Chang-Goo Kim, Eliot Quataert, John C. Forbes, Claude-André Faucher-Giguère, Robert Feldmann, Zachary Hafen, Philip F. Hopkins, Dušan Kereš, Norman Murray, Andrew Wetzel
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Accepted to MNRAS with minor revisions, main body is 25 pages with 14 figures
We characterize mass, momentum, energy and metal outflow rates of multi-phase galactic winds in a suite of FIRE-2 cosmological "zoom-in" simulations from the Feedback in Realistic Environments (FIRE) project. We analyze simulations of low-mass dwarfs, intermediate-mass dwarfs, Milky Way-mass halos, and high-redshift massive halos. Consistent with previous work, we find that dwarfs eject about 100 times more gas from their interstellar medium (ISM) than they form in stars, while this mass "loading factor" drops below one in massive galaxies. Most of the mass is carried by the hot phase ($>10^5$ K) in massive halos and the warm phase ($10^3-10^5$ K) in dwarfs; cold outflows ($<10^3$ K) are negligible except in high-redshift dwarfs. Energy, momentum and metal loading factors from the ISM are of order unity in dwarfs and significantly lower in more massive halos. Hot outflows have $2-5\times$ higher specific energy than needed to escape from the gravitational potential of dwarf halos; indeed, in dwarfs, the mass, momentum, and metal outflow rates increase with radius whereas energy is roughly conserved, indicating swept up halo gas. Burst-averaged mass loading factors tend to be larger during more powerful star formation episodes and when the inner halo is not virialized, but we see effectively no trend with the dense ISM gas fraction. We discuss how our results can guide future controlled numerical experiments that aim to elucidate the key parameters governing galactic winds and the resulting associated preventative feedback.
Characterization of molecular outflows at core-scale in the massive clump AGAL G345.0029-0.224
Instituto de Astronomía y Física del Espacio, CONICET-UBA（空间天体物理与物理研究所，阿根廷国家科学研究委员会-布宜诺斯艾利斯大学）；Departamento de Física, Facultad de Ciencias Exactas y Naturales, UBA（布宜诺斯艾利斯大学理学院物理系）；Universidad Nacional Autónoma de México, Instituto de Ciencias Nucleares（墨西哥国立自治大学核科学学院）
The effects of LMC-mass environments on their dwarf satellite galaxies in the FIRE simulations
描述像大麦云（LMC）这样的矮星系的预测环境变得越来越重要，因为下一代的调查将灵敏度限制在宇宙学距离的低质量区域。我们研究的环境影响的LMC质量晕（$M_{200m} \sim 10^{11}$ M $_\odot$）对他们的人口的卫星（$M_\star \geq 10^4$ M $_\odot$）使用一套放大模拟在现实环境中的反馈（FIRE）项目。我们的模拟预测显著的热电晕与$T\sim10^5$ K和$M_\text{gas}\sim10^{9.5}$ M $_\odot$。我们确定了矮卫星星系，特别是中等质量的卫星（$M_\star = 10^{6-7}$ M $_\odot$）的环境淬火的签名。这些天体的气体含量表明，冲压压力可能是淬火机制，有时还得到恒星形成反馈的帮助。LMC质量宿主的卫星重复了MW质量宿主卫星中发现的静止分数的恒星质量依赖性（即静止分数随着恒星质量的减小而增加）。与附近中心的强烈双峰猝灭时间分布相比，LMC-质量宿主的Saxons具有更广泛的猝灭时间。最后，我们确定了显着的潮汐恒星结构周围的四个我们的六个LMC类似物，这表明恒星流可能是常见的。这些潮汐特征起源于近轨道的卫星，延伸到距离中央星系80 kpc的$\sim$，包含$\sim10^{6-7}$ M $_\odot$ ~的恒星。
CLASSY. XV. Kinematics and Spatial Distributions of Outflows in Local Highly Star-Forming Galaxies
Minnesota Institute for Astrophysics, University of Minnesota（明尼苏达大学天体物理研究所）；Department of Astronomy, The University of Michigan（密歇根大学天文学系）；Center for Cosmology and Computational Astrophysics, Institute for Advanced Study in Physics, Zhejiang University（浙江大学物理学院宇宙学与计算天文中心）；Institute of Astronomy, School of Physics, Zhejiang University（浙江大学物理学院天体物理研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Center for Astrophysical Sciences, Department of Physics & Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学物理与天文系天体物理科学中心）；Stockholm University, Department of Astronomy and Oskar Klein Centre for Cosmoparticle Physics, AlbaNova University Centre（斯德哥尔摩大学奥斯卡·克莱因宇宙粒子物理中心天文学系阿尔巴诺瓦大学中心）；Department of Physics and Astronomy, Northwestern University（西北大学物理与天文系）
3-D gas-phase elemental abundances across the formation histories of Milky Way-mass galaxies in the FIRE simulations: initial conditions for chemical tagging
Empirical Calibration of Na I D and Other Absorption Lines as Tracers of High-Redshift Neutral Outflows
Università di Bologna（博洛尼亚大学）；The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森天体物理中心）；INAF, Astrophysics and Space Science Observatory（意大利国家天体物理研究所，天体物理与空间科学观测站）；Caltech/IPAC（加州理工学院/IPAC）；National Centre for Nuclear Research（国家核研究中心）；SISSA（的里雅斯特高级研究学院）
研究通过实证校准Na I D及其他吸收线，以更准确地估算高红移中性喷流的质量和流量，发现Na I校准与本地关系接近，但Mg II校准存在显著差异，可能与尘埃贫乏有关。
Widespread Extended [CII] Emission in High-Redshift Galaxies: Insights from the FIRE-2 Cosmological Zoom-in Simulations
California Institute of Technology（加州理工学院）；CIERA and Department of Physics and Astronomy, Northwestern University（西北大学 CIERA 与物理和天文系）；IPAC, California Institute of Technology（加州理工学院 IPAC）；Department of Physics and Astronomy, University of Pennsylvania（宾夕法尼亚大学物理和天文系）
Disk Wind Feedback from High-mass Protostars. V. Application of Multi-Modal Machine Learning to Characterize Outflow Properties
Canadian Institute for Theoretical Astrophysics, University of Toronto（加拿大理论天体物理研究所，多伦多大学）；Department of Astronomy, University of Virginia（弗吉尼亚大学天文学系）；Department of Astronomy, Columbia University（哥伦比亚大学天文学系）；Department of Astronomy, University of Wisconsin-Madison（威斯康星大学麦迪逊分校天文学系）；Department of Statistical Sciences, University of Toronto（多伦多大学统计科学系）；David A. Dunlap Department of Astronomy & Astrophysics, University of Toronto（多伦多大学大卫·A·邓普天文与天体物理系）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普天文与天体物理研究所）；Data Sciences Institute, University of Toronto（多伦多大学数据科学研究所）；Department of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院天文学系）；State Key Laboratory of Dark Matter Physics, School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院暗物质物理全国重点实验室）
Properties of Galactic Outflows Driven by Starburst at Cosmic Noon: Insights from Hydrodynamical Simulations
School of Physics and Astronomy, Sun Yat-Sen University（中山大学物理与天文学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area（粤港澳大湾区空间科学中心）
A deep, multi-epoch Chandra HETG study of the ionized outflow from NGC 4051
主动吸积的超大质量黑洞显著影响其宿主星系的演化，通过以广角流出排出大部分气体来截断进一步的恒星形成。X射线波段是理解这些黑洞风如何影响其环境的关键，因为流出物具有高温（$\sim$ 10 $^{5-8}$ K）。我们已经开发了一个贝叶斯框架，用于表征活动星系核（AGN）的外流，具有更好的探索参数空间和进行鲁棒模型选择的能力。我们将这个框架应用到一个新的700 ks和档案315 ks钱德拉高能透射光栅观测的塞弗特星系NGC 4051。我们已经检测到NGC 4051的六个固有吸收体。这些风分量的速度跨度从400 km s $^{-1}$到30，000 km s $^{-1}$。我们已经确定，统计上最重要的风分量是纯粹的碰撞电离，这是第一次检测到这样的吸收体。这种风具有$T\approx10^7$ K和$v\approx880$ km s $^{-1}$，并且在两个时期之间保持非常稳定。其他慢分量也随时间保持稳定。快速外流成分在2008年至2016年之间改变了它们的性质，这表明要么是物理变化，要么是云在视线范围内移动。对于其中一个快速分量，我们获得了迄今为止最严格的风密度测量值之一，log $n/$ [cm $^{-3}$ ]=13.0 $^{+0.01}_{-0.02}$，并确定它位于$\sim$ 240引力半径处。估计总流出功率超过5%的热光度（尽管有很大的不确定性），使其在星系-黑…
