MIGHTEE-HI: the HI Size-Mass relation over the last billion years
Sambatriniaina H. A. Rajohnson, Bradley S. Frank, Anastasia A. Ponomareva, Natasha Maddox, Renée C. Kraan-Korteweg, Matt J. Jarvis, Elizabeth A. K. Adams, Tom O… 展开作者
Sambatriniaina H. A. Rajohnson, Bradley S. Frank, Anastasia A. Ponomareva, Natasha Maddox, Renée C. Kraan-Korteweg, Matt J. Jarvis, Elizabeth A. K. Adams, Tom Oosterloo, Maarten Baes, Kristine Spekkens, Nathan J. Adams, Marcin Glowacki, Sushma Kurapati, Isabella Prandoni, Ian Heywood, Jordan D. Collier, Srikrishna Sekhar, Russ Taylor
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10 pages, 5 figures, accepted for publication in MNRAS
We present the observed HI size-mass relation of $204$ galaxies from the MIGHTEE Survey Early Science data. The high sensitivity of MeerKAT allows us to detect galaxies spanning more than 4 orders of magnitude in HI mass, ranging from dwarf galaxies to massive spirals, and including all morphological types. This is the first time the relation has been explored on a blind homogeneous data set which extends over a previously unexplored redshift range of $0 < z < 0.084$, i.e. a period of around one billion years in cosmic time. The sample follows the same tight logarithmic relation derived from previous work, between the diameter ($D_{\rm HI}$) and the mass ($M_{\rm HI}$) of HI discs. We measure a slope of $0.501\pm 0.008$, an intercept of $-3.252^{+0.073}_{-0.074}$, and an observed scatter of $0.057$ dex. For the first time, we quantify the intrinsic scatter of $0.054 \pm 0.003$ dex (${\sim} 10 \%$), which provides a constraint for cosmological simulations of galaxy formation and evolution. We derive the relation as a function of galaxy type and find that their intrinsic scatters and slopes are consistent within the errors. We also calculate the $D_{\rm HI} - M_{\rm HI}$ relation for two redshift bins and do not find any evidence for evolution with redshift. These results suggest that over a period of one billion years in lookback time, galaxy discs have not undergone significant evolution in their gas distribution and mean surface mass density, indicating a lack of dependence on both morphological type and redshift.
Decomposing the growth mechanisms of galaxies over the last 10 billion years
The University of Western Australia（西澳大学）；University of Southampton（南安普顿大学）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布拉拉天文台）；EPFL Laboratory of Astrophysics (LASTRO)（洛桑联邦理工学院天体物理学实验室）；NAF-Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Sydney Institute for Astronomy, School of Physics, University of Sydney（悉尼大学物理学院天文学研究所）；Department of Astrophysics, University of Vienna（维也纳大学天体物理系）
CHILES XI: Resolved HI morphologies and the evolution of the H2/HI ratio over the last five billion years
National Radio Astronomy Observatory（美国国家射电天文台）；Department of Astronomy, Columbia University（哥伦比亚大学天文学系）；Department of Physics, Montana State University（蒙大拿州立大学物理学系）；Department of Astronomy, University of Cape Town（开普敦大学天文学系）；Department of Astronomy, University of Massachusetts（马萨诸塞大学天文学系）；Department of Space, Earth and Environment, Chalmers University of Technology（查尔姆斯理工大学空间、地球与环境系）；ASTRON, the Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；Department of Physics, Virginia Tech（弗吉尼亚理工学院物理学系）；Department of Astronomy, Yonsei University（延世大学天文学系）
The VIMOS Public Extragalactic Redshift Survey (VIPERS): Downsizing of the blue cloud and the influence of galaxy size on mass quenching over the last eight billion years
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。
JADES: Differing assembly histories of galaxies -- Observational evidence for bursty SFHs and (mini-)quenching in the first billion years of the Universe
The assembly history of NGC 1365 through chemical archaeology
Institute for Theory & Computation, Center for Astrophysics — Harvard & Smithsonian（哈佛-史密森尼天体物理中心理论计算研究所）；Research School for Astronomy & Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australian National University（澳大利亚国立大学三维全天空天体物理学卓越研究中心）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Department of Astronomy, University of Virginia（弗吉尼亚大学天文学系）；Virginia Institute for Theoretical Astronomy, University of Virginia（弗吉尼亚大学理论天文学研究所）；The Observatories, Carnegie Institution for Science（卡内基科学机构天文台）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）
通过分析 NGC 1365 的高分辨率氧丰度并结合 IllustrisTNG 模拟，揭示星系盘、棒和气体盘分别由不同时期合并事件组装的历史，证明化学考古学可追踪星系动力学演化。
Semi-empirical constraints on the HI mass function of star-forming galaxies and $Ω_{\rm HI}$ at $z\sim 0.37$ from interferometric surveys
Université de Genève（日内瓦大学）；University of Zurich（苏黎世大学）；Università degli Studi di Padova（帕多瓦大学）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；University of the Western Cape（西开普敦大学）
