Despite the existence of well-defined relationships between cold gas and star formation, there is evidence that some galaxies contain large amounts of HI that do not form stars efficiently. By systematically assessing the link between HI and star formation within a sample of galaxies with extremely high HI masses (log M_HI/M_sun > 10), we uncover a population of galaxies with an unexpected combination of high HI masses and low specific star formation rates that exists primarily at stellar masses greater than log M_*/M_sun ~ 10.5. We obtained HI maps of 20 galaxies in this population to understand the distribution of the HI and the physical conditions in the galaxies that could be suppressing star formation in the presence of large quantities of HI. We find that all of the galaxies we observed have low HI surface densities in the range in which inefficient star formation is common. The low HI surface densities are likely the main cause of the low sSFRs, but there is also some evidence that AGN or bulges contribute to the suppression of star formation. The sample's agreement with the global star formation law highlights its usefulness as a tool for understanding galaxies that do not always follow expected relationships.
A New Metal-poor Globular Cluster and Resolved Stars in the Outer Disk of the Black Eye Galaxy M64: Implication for the Origin of the Type III Disk Break
GLACE survey: OSIRIS/GTC multi-object spectroscopy of the rich galaxy cluster ZwCl 0024.0+1652 at z~0.4. III. The mass-SFR relation and the quenching of cluster galaxies
Institut de Radioastonomie Millimétrique (IRAM)（毫米波射电天文学研究所）；Universidad de Granada（格拉纳达大学）；Asociación Astrofísica para la Promoción de la Investigación, Instrumentación y su Desarrollo, ASPID（天文研究、仪器及其发展促进协会）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna (ULL)（拉古纳大学）；Fundación Galileo Galilei-INAF（伽利略基金会-意大利国家天体物理研究所）；ISDEFE；Instituto Carlos I de Física Teórica y Computacional, Universidad de Granada（格拉纳达大学卡洛斯一世理论与计算物理研究所）；Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理研究所）；Instituto de Astronomía, Universidad Nacional Autónoma de México (UNAM)（墨西哥国立自治大学天文学研究所）；Centro de Astrobiología (CSIC/INTA)（天体生物学中心）；Universidad Complutense de Madrid（马德里康普顿斯大学）；Telespazio UK for European Space Agency, European Space Astronomy Centre（欧洲空间局欧洲空间天文中心）；Instituto de Física de Cantabria (CSIC-Universidad de Cantabria)（坎塔布里亚物理研究所）；Kotebe University of Education（科特贝教育大学）；Space Science and Geospatial Institute (SSGI)（空间科学与地理空间研究所）；Mbarara University of Science and Technology (MUST)（姆巴拉拉科技大学）
Self-interacting dark matter delays bar growth in an isolated gas-rich galactic disk: torque-resolved numerical evidence
Intelligent Manufacturing College, Zhejiang Guangsha Vocational and Technical University of Construction（浙江广厦建设职业技术大学智能制造学院）；Institute of Theoretical Physics, Chinese Academy of Sciences（中国科学院理论物理研究所）
Light curve spectral energy distribution fitting of 13 carbon-rich Mira variables stars in the Small Magellanic Cloud
National and Kapodistrian University of Athens（雅典国立卡波迪斯特里安大学）；Università 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 Geneva（日内瓦大学）；Koninklijke Sterrenwacht van België（比利时皇家天文台）；SISSA（的里雅斯特国际高等研究学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）
