MIGHTEE-HI: The relation between the HI gas in galaxies and the cosmic web
Madalina N. Tudorache, M. J. Jarvis, I. Heywood, A. A. Ponomareva, N. Maddox, B. S. Frank, N. J. Adams, R. A. A. Bowler, I. H. Whittam, M. Baes, H. Pan, S. H. A… 展开作者
Madalina N. Tudorache, M. J. Jarvis, I. Heywood, A. A. Ponomareva, N. Maddox, B. S. Frank, N. J. Adams, R. A. A. Bowler, I. H. Whittam, M. Baes, H. Pan, S. H. A. Rajohnson, F. Sinigaglia, K. Spekkens
备注：
11 pages, 9 figures, 5 tables, accepted for publication in MNRAS
We study the 3D axis of rotation (3D spin) of 77 HI galaxies from the MIGHTEE-HI Early Science observations, and its relation to the filaments of the cosmic web. For this HI-selected sample, the alignment between the spin axis and the closest filament ($\lvert \cos ψ\rvert$) is higher for galaxies closer to the filaments, with $\langle\lvert \cos ψ\rvert\rangle= 0.66 \pm 0.04$ for galaxies $<5$ Mpc from their closest filament compared to $\langle\lvert \cos ψ\rvert\rangle= 0.37 \pm 0.08$ for galaxies at $5 < d <10$ Mpc. We find that galaxies with a low HI-to-stellar mass ratio ($\log_{10}(M_{\rm HI}/M_{\star}) < 0.11$) are more aligned with their closest filaments, with $\langle\lvert \cos ψ\rvert\rangle= 0.58 \pm 0.04$; whilst galaxies with ($\log_{10}(M_{\rm HI}/M_{\star}) > 0.11$) tend to be mis-aligned, with $\langle\lvert \cos ψ\rvert\rangle= 0.44 \pm 0.04$. We find tentative evidence that the spin axis of HI-selected galaxies tend to be aligned with associated filaments ($d<10$ Mpc), but this depends on the gas fractions. Galaxies that have accumulated more stellar mass compared to their gas mass tend towards stronger alignment. Our results suggest that those galaxies that have accrued high gas fraction with respect to their stellar mass may have had their spin axis alignment with the filament disrupted by a recent gas-rich merger, whereas the spin vector for those galaxies in which the neutral gas has not been strongly replenished through a recent merger tend to orientate towards alignment with the filament. We also investigate the spin transition between galaxies with a high HI content and a low HI content at a threshold of $M_{\mathrm{HI}}\approx 10^{9.5} M_{\odot}$ found in simulations, however we find no evidence for such a transition with the current data.
MIGHTEE-HI: Environmental effects of cosmic filaments on extragalactic HI detections in the COSMOS and XMM-LSS fields
University of Oxford（牛津大学）；University of Cambridge（剑桥大学）；University of the Western Cape（西开普敦大学）；University of Bristol（布里斯托大学）；Universiteit Gent（根特大学）；University of Edinburgh（爱丁堡大学）；Inter-University Institute for Data Intensive Astronomy, Department of Astronomy, University of Cape Town（开普敦大学天文学系数据密集型天文跨大学研究所）；Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University（大学物理、天文与数学学院天体物理学研究中心）
MIGHTEE: The evolving radio luminosity functions of star-forming galaxies to $z\sim 4.5$ and the cosmic history of star formation
University of Oxford（牛津大学）；UKRI STFC Rutherford Appleton Laboratory（英国研究与创新部STFC拉瑟福德阿普尔顿实验室）；University of the Western Cape（西开普大学）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；Carnegie Observatories（卡内基观测站）；Rhodes University（罗德兹大学）
Star-forming galaxies in the cosmic web in the last 11 Gyr
Observatoire Astronomique de Strasbourg, UMR 7550, CNRS, Université de Strasbourg（斯特拉斯堡天文台）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Department of Physics and Astronomy, University of the Western Cape（西开普大学物理与天文学系）
Tracing the Cosmic web across Cosmic time through SKA observations of radio galaxies
National Centre for Nuclear Research（国家核研究中心）；University of Tartu（塔尔图大学）；Assam Don Bosco University（阿萨姆唐博斯科大学）；Observatoire de Paris（巴黎天文台）；Collège de France（法兰西公学院）；PSL University（PSL大学）；Sorbonne University（索邦大学）
Learning the Cosmic Web: Graph-based Classification of Simulated Galaxies by their Dark Matter Environments
University College London（伦敦大学学院）；University of Portsmouth（朴茨茅斯大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）
Impact of Cosmic Filaments on Galaxy Morphological Evolution and Predictions of Early Cosmic Web Structure for Roman
Space Telescope Science Institute（太空望远镜科学研究所）；New Mexico State University（新墨西哥州立大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学加拿大理论天体物理研究所）；Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学哥伦比亚天体物理学实验室）；Johns Hopkins University（约翰斯·霍普金斯大学）
CHILES VI: HI and H$α$ Observations for z < 0.1 Galaxies; Probing HI Spin Alignment with Filaments in the Cosmic Web
我们目前的中性氢（HI）和电离氢（H $α$）的观测10个星系的红移为0.1。HI观测来自COSMOS HI大型河外巡天（智利）的第一个纪元（178小时）。我们的样本是HI偏置的，由10个晚型星系组成，HI质量范围从$1.8\times10^{7}$ M $_{\odot}$到$1.1\times10^{10}$ M $_{\odot}$。我们发现，虽然大多数星系的形态和运动学的不规则性，他们一般遵循的标度关系中发现的较大的样本。我们发现，HI和H $α$速度达到旋转曲线的平坦部分。我们确定的大尺度结构在附近的智利体积使用DisPerSE与光谱目录从SDSS。我们探索的气体性质的星系作为一个功能的位置在宇宙网络。我们还比较了角动量矢量（自旋）的星系最近的宇宙网丝的方向。我们的研究结果表明，星系自旋往往与宇宙网细丝对齐，并显示出与自旋角对齐相关的过渡质量的暗示。
CWITools: A Python3 Data Analysis Pipeline for the Cosmic Web Imager Instruments
Palomar Cosmic Web Imager（PCWI）和Keck Cosmic Web Imager（KCWI）是Palomar天文台的Hale 5米望远镜和W. M. Keck Observatory天文台近年来，这些仪器越来越多地用于进行调查工作，特别是在高红移的环星系和星系间介质的重点。从三维IFU数据中提取微弱信号是一项复杂的任务，如果没有适当的工具，对于大样本可能会变得非常困难。我们提出了CWITools，一个用Python 3编写的软件包，用于分析PCWI和KCWI数据。CWITools旨在提供标准仪器数据简化管道的输出与科学产品之间的管道，如表面亮度图，光谱，速度图以及各种相关模型和测量。虽然该软件包是专门为PCWI和KCWI数据设计的，但该软件包是开源的，可以适应任何三维积分场光谱数据。在这里，我们将描述这个管道，各个步骤背后的方法，并提供示例应用程序。
