MUSE Analysis of Gas around Galaxies (MAGG) -- II: Metal-enriched halo gas around z~1 galaxies
Rajeshwari Dutta, Michele Fumagalli, Matteo Fossati, Emma K. Lofthouse, J. Xavier Prochaska, Fabrizio Arrigoni Battaia, Richard M. Bielby, Sebastiano Cantalupo,… 展开作者
Rajeshwari Dutta, Michele Fumagalli, Matteo Fossati, Emma K. Lofthouse, J. Xavier Prochaska, Fabrizio Arrigoni Battaia, Richard M. Bielby, Sebastiano Cantalupo, Ryan J. Cooke, Michael T. Murphy, John M. O'Meara
We present a study of the metal-enriched cool halo gas traced by MgII absorption around 228 galaxies at z~0.8-1.5 within 28 quasar fields from the MUSE Analysis of Gas around Galaxies (MAGG) survey. We observe no significant evolution in the MgII equivalent width versus impact parameter relation and in the MgII covering fraction compared to surveys at z<~0.5. The stellar mass, along with distance from galaxy centre, appears to be the dominant factor influencing the MgII absorption around galaxies. With a sample that is 90% complete down to a star formation rate of ~0.1 Msun/yr and up to impact parameters ~250-350 kpc from quasars, we find that the majority (67^{+12}_{-15}% or 14/21) of the MgII absorption systems are associated with more than one galaxy. The complex distribution of metals in these richer environments adds substantial scatter to previously-reported correlations. Multiple galaxy associations show on average five times stronger absorption and three times higher covering fraction within twice the virial radius than isolated galaxies. The dependence of MgII absorption on galaxy properties disfavours the scenario in which a widespread intra-group medium dominates the observed absorption. This leaves instead gravitational interactions among group members or hydrodynamic interactions of the galaxy haloes with the intra-group medium as favoured mechanisms to explain the observed enhancement in the MgII absorption strength and cross section in rich environments.
MUSE Analysis of Gas around Galaxies (MAGG) -- VII. Emission line galaxies near strong blended Ly$α$ absorption systems at $z\gtrsim3$
Università degli Studi di Milano-Bicocca（米兰比可卡大学）；INAF – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INAF – Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Aix Marseille Universite, CNRS, CNES, LAM（艾克斯马赛大学）
MUSE Analysis of Gas around Galaxies (MAGG) -- V: Linking ionized gas traced by CIV and SiIV absorbers to Ly$α$ emitting galaxies at $z\approx 3.0-4.5$
MUSEQuBES: Physical conditions, origins, and multi-element abundances of the circumgalactic medium of an isolated, star-forming dwarf galaxy at z=0.57
University of Michigan（密歇根大学）；Inter-University Centre for Astronomy & Astrophysics（天文学与天体物理学跨大学中心）；The Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；University of North Texas（北德克萨斯大学）；Tsinghua University（清华大学）；The University of Chicago（芝加哥大学）；Northwestern University（西北大学）；Tel Aviv University（特拉维夫大学）
MUSEQuBES: Investigating the Physical and Chemical Properties of Circumgalactic Gas Around Ly$α$ Emitters at $z \approx 3.3$
IUCAA（印度天体物理研究与教育中心）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；Department of Physics, University of Milan Bicocca（米兰比可卡大学物理学系）
Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra I cluster III. Untangling UDG 32 from the stripped filaments of NGC 3314A with multi-wavelength data
Heavy elements unveil the non primordial origin of the giant HI ring in Leo
狮子座环是本宇宙中已知的最大的河外中性云，其起源和命运在发现38年后仍有争议。它的存在也可以归因于残留的原始气体，其中含有一些低水平的金属污染，而不是在星系-星系相遇期间剥离的富集气体。利用VLT上的MUSE（Multi Unit Spectroscopic Explorer）探测器，我们对狮子座环中的3个HI团簇进行了光学积分场谱研究，首次探测到环中的电离氢，并确定了4个由大质量恒星提供能量的星云区。这些星云显示了几条金属线（[OIII]，[NII]，[SII]），这些金属线允许可靠的测量金属丰度，发现接近或高于太阳值。考虑到弥散恒星对应物的微弱性，在观测到的重元素中，只有不到3%的重元素可能是在环的主体中局部产生的，而在朝向M96的HI团簇中产生的重元素不超过15%。这个推论，以及这些区域之间的化学同质性，令人信服地证明了环中的气体不是原始的，而是在星系盘中预先富集的，然后被潮汐力移除和塑造，形成了稀疏的恒星群。
The "bubbly" interstellar medium as origin for the inhomogeneous internal metallicity distributions in large disk galaxies
The University of Melbourne（墨尔本大学）；California Institute of Technology（加州理工学院）；The Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）
The KAGG survey: KCWI Analysis of Gas around Galaxies at z~3-5
The University of Oklahoma（俄克拉荷马大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Kavli Institute for the Physics and Mathematics of the Universe（柯利宇宙物理与数学研究所）；National Astronomical Observatory of Japan（日本国立天文台）；National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（塔塔基础研究院国家射电天文学中心）；National Radio Astronomy Observatory（美国国家射电天文台）；Maria Mitchell Observatory（玛丽亚·米切尔天文台）；University of California, Merced（加州大学默塞德分校）；Università degli Studi di Milano-Bicocca（米兰比可卡大学）
