On the Evolution of the Velocity-Mass-Size Relations of Disk-Dominated Galaxies over the Past 10 Billion Years
Aaron A. Dutton, Frank C. van den Bosch, S. M. Faber, Luc Simard, Susan A. Kassin, David C. Koo, Kevin Bundy, Jiasheng Huang, Benjamin J. Weiner, Michael C. Coo… 展开作者
Aaron A. Dutton, Frank C. van den Bosch, S. M. Faber, Luc Simard, Susan A. Kassin, David C. Koo, Kevin Bundy, Jiasheng Huang, Benjamin J. Weiner, Michael C. Cooper, Jeffrey A. Newman, Mark Mozena, Anton Koekemoer
备注：
19 pages, 10 figures, accepted to MNRAS, minor changes to previous version
We study the evolution of the scaling relations between maximum circular velocity, stellar mass and optical half-light radius of star-forming disk-dominated galaxies in the context of LCDM-based galaxy formation models. Using data from the literature combined with new data from the DEEP2 and AEGIS surveys we show that there is a consistent observational and theoretical picture for the evolution of these scaling relations from z\sim 2 to z=0. The evolution of the observed stellar scaling relations is weaker than that of the virial scaling relations of dark matter haloes, which can be reproduced, both qualitatively and quantitatively, with a simple, cosmologically-motivated model for disk evolution inside growing NFW dark matter haloes. In this model optical half-light radii are smaller, both at fixed stellar mass and maximum circular velocity, at higher redshifts. This model also predicts that the scaling relations between baryonic quantities evolve even more weakly than the corresponding stellar relations. We emphasize, though, that this weak evolution does not imply that individual galaxies evolve weakly. On the contrary, individual galaxies grow strongly in mass, size and velocity, but in such a way that they move largely along the scaling relations. Finally, recent observations have claimed surprisingly large sizes for a number of star-forming disk galaxies at z \sim 2, which has caused some authors to suggest that high redshift disk galaxies have abnormally high spin parameters. However, we argue that the disk scale lengths in question have been systematically overestimated by a factor \sim 2, and that there is an offset of a factor \sim 1.4 between Hαsizes and optical sizes. Taking these effects into account, there is no indication that star forming galaxies at high redshifts (z\sim 2) have abnormally high spin parameters.
Weak Evolution of Cosmic Atomic Hydrogen over the Past 4.5 Billion Years
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Shanghai Jiao Tong University（上海交通大学）；Guizhou University（贵州大学）；University College London（伦敦大学学院）；Max Planck Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；University of Edinburgh（爱丁堡大学）；University of Chinese Academy of Sciences（中国科学院大学）
The Atacama Cosmology Telescope: stellar mass growth in massive galaxy clusters from DR5 over the past 7 billion years
University of the Witwatersrand（威特沃特斯兰德大学）；National Centre for Nuclear Research（国家核研究中心）；University of KwaZulu-Natal（夸祖鲁-纳塔尔大学）；Rutgers, the State University of New Jersey（新泽西州立罗格斯大学）；Institute of Space Sciences (ICE-CSIC)（空间科学研究所）
Neutral Atomic Hydrogen in a Star-forming Galaxy 7 Billion Years Ago
University of the Witwatersrand（威特沃特斯兰德大学）；University of Pretoria（比勒陀利亚大学）；Rhodes University（罗德岛大学）；South African Radio Astronomy Observatory（南非射电天文观测台）；University of Western Australia（西澳大利亚大学）；SKA Observatory（平方公里阵列望远镜观测站）；University of Oxford（牛津大学）
On the Last 10 Billion Years of Stellar Mass Growth in Star-Forming Galaxies
恒星形成率-恒星质量关系（SFR-M*）及其演化（即，SFR主序）描述了给定恒星质量和给定红移的星系的增长率。假设现在的恒星形成星系在过去总是恒星形成的，这些增长率观测可以被整合来计算平均恒星形成历史（SFH）。使用这种主序列积分（MSI）方法，我们可以追溯到现在的大质量恒星形成星系，当它们是当前恒星质量的10-20%时。在这些时期的整合是强大的：支持我们的计算的SFR数据是一致的恒星质量密度在这个政权的演变。这些SFH的分析近似。基于积分的结果重申了以前的建议，即目前的恒星形成星系形成几乎所有的恒星质量在z <2. It follows that massive galaxies observed at z>2不是典型的祖先恒星形成星系今天。我们还检查基于MSI的SFH对那些从化石记录的分析推断-从光谱能量分布（SED）的恒星形成星系在斯隆数字巡天，和色星等图（CMD）的矮不规则星系解决恒星。一旦考虑到恒星星族年龄的不确定性，主序列与基于SED的SFH（来自VESPA）非常一致。外推SFR主序星观测到矮星系，我们发现的ACS附近的星系巡天金库和本星系群星系的CMD分析的MSI结果和SFH之间的差异。解析出的矮星系似乎比主序列趋势所暗示的要慢得多，也比质量稍高的SED分析星系慢。这种差异可能标志着SFH测定的问题，但它也可能标志着在最低恒星质量下恒星形成趋势的转变。
The Growth of Dust in Galaxies in the First Billion Years with Applications to Blue Monsters
University of Florida（佛罗里达大学）；Cosmic Dawn Center at the Niels Bohr Institute, University of Copenhagen and DTU-Space, Technical University of Denmark（哥本哈根大学尼尔斯·玻尔研究所黎明中心及丹麦技术大学DTU空间）；University of Virginia（弗吉尼亚大学）；Virginia Institute for Theoretical Astronomy, University of Virginia（弗吉尼亚理论天文学研究所）；The NSF-Simons AI Institute for Cosmic Origins, USA（美国NSF-西蒙斯宇宙起源人工智能研究所）；University of California（加州大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校宇宙前沿中心）；University of Bologna（博洛尼亚大学）；INAF, Astrophysics and Space Science Observatory Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；Universi（大学）
