Disk Turbulence and Star Formation Regulation in High$-z$ Main Sequence Analogue Galaxies
Laura Lenkić, Deanne B. Fisher, Alberto D. Bolatto, Peter J. Teuben, Rebecca C. Levy, Jiayi Sun, Rodrigo Herrera-Camus, Karl Glazebrook, Danail Obreschkow, Roberto Abraham
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24 pages, 12 figures, 2 tables, accepted for publication in The Astrophysical Journal
The gas-phase velocity dispersions in disk galaxies, which trace turbulence in the interstellar medium, are observed to increase with lookback time. However, the mechanisms that set this rise in turbulence are observationally poorly constrained. To address this, we combine kiloparsec-scale ALMA observations of CO(3-2) and CO(4-3) with HST observations of H$α$ to characterize the molecular gas and star formation properties of seven local analogues of main sequence galaxies at $z \sim 1-2$, drawn from the DYNAMO sample. Investigating the ''molecular gas main sequence'' on kpc-scales, we find that galaxies in our sample are more gas-rich than local star-forming galaxies at all disk positions. We measure beam smearing corrected molecular gas velocity dispersions and relate them to the molecular gas and star formation rate surface densities. Despite being relatively nearby ($z \sim 0.1$), DYNAMO galaxies exhibit high velocity dispersions and gas and star formation rate surface densities throughout their disks, when compared to local star forming samples. Comparing these measurements to predictions from star formation theory, we find very good agreements with the latest feedback-regulated star formation models. However, we find that theories which combine gravitational energy dissipation from radial gas transport with feedback over-estimate the observed molecular gas velocity dispersions.
Turbulence modes in molecular clouds in M33: a challenging test of the Brunt-Federrath framework
Institute of Astronomy, National Tsing Hua University（国立清华大学天文研究所）；Department of Physics, Graduate School of Science, Osaka Metropolitan University（大阪公立大学理学研究科物理系）；Astronomical Institute, Tohoku University（东北大学天文学研究所）；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学天体物理研究所）；Global Banking School, Universal Square, Devonshire Street North, Manchester, M12 6JH, UK（曼彻斯特环球银行学院）；Armagh Observatory and Planetarium（阿马赫天文台和行星馆）；Subatomic Physics Research Group, Science and Technology Advanced Institute, Van Lang University（万朗大学科技先进学院亚原子物理研究组）；Faculty of Applied Technology, Van Lang School of Technology, Van Lang University（万朗大学技术学院应用技术系）
Cascading from the winds to the disk: the universality of supernovae-driven turbulence in different galactic interstellar media
University of California, Santa Cruz（加州大学圣克鲁兹分校）；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）；Princeton University（普林斯顿大学）
The driving mode of turbulence in disc galaxy simulations with adaptive mesh refinement
Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Lund Observatory, Division of Astrophysics, Department of Physics, Lund University（隆德大学物理系天体物理学部隆德天文台）
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）
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）
