Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at $1.5 < z < 6.4$
K. B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda, T. Nanayakkara, R. Bacon, L. A. Boogaard, S. Conseil, T. Contini, E. C. Herenz, W. K… 展开作者
K. B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda, T. Nanayakkara, R. Bacon, L. A. Boogaard, S. Conseil, T. Contini, E. C. Herenz, W. Kollatschny, M. Krumpe, F. Leclercq, G. Mahler, J. Matthee, V. Mauerhofer, J. Richard, J. Schaye
备注：
Accepted by A&A. Contains 54 pages, 21 figures, and appendices. Catalogs described in Tables B.1 and C.1 will be made available with published paper
静止帧紫外线发射线探测发射恒星的星系及其环境的物理参数。最强的主紫外线，Ly $α$，一直在推进早期宇宙星系形成的一般知识。然而，当CGM和IGM的中性氢分数增加时，在$z \gtrsim 6$处观察Ly $α$发射变得越来越具有挑战性。次级弱紫外发射线为研究高红移星系的性质提供了重要的替代方法。我们提出了一个大样本的静止框架中红移的紫外发射线源的校准和探索次级紫外线和发射星系的物理性质和它们的Ly $α$发射之间的联系。通过三维MUSE数据立方体中的非目标源检测，选择了具有$1.5 < z < 6.4$的2052个发射线源的样本。我们通过发射线模板匹配搜索最佳提取的完整样品的UV发射特征的1D光谱，从而得到100多个静止帧UV发射线检测的样品。我们发现，（非赖氨酸$α$）紫外发射线的检测效率随调查深度的增加，和紫外发射线的强度往往与Ciii]的强度。我们测量了共振发射线相对于系统示踪剂的速度偏移以及电子密度和气相丰度。最后，利用“光电离模型概率密度函数”，我们发现紫外线发射体的电离参数log 10（U）$\approx$-2.5和金属质量分数分布在Z $\approx$ 10 $^{-2}$附近，即Z $\approx$ 0.66 Z $\odot$。本文提供了本工作中研究的MUSE物体完整样本的增值目录以及文献中的紫外线发射器集合。
英文摘要：
[Abbreviated] Rest-frame UV emission lines probe physical parameters of the emitting star-forming galaxies and their environments. The strongest main UV line, Ly$α$, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Ly$α$ emission becomes increasingly challenging at $z \gtrsim 6$ when the neutral hydrogen fraction of the CGM and IGM increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies' physical properties and their Ly$α$ emission. The sample of 2052 emission line sources with $1.5 < z < 6.4$ was selected through untargeted source detection in three-dimensional MUSE data cubes. We searched optimally extracted 1D spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Ly$α$) UV emission lines increases with survey depth, and that the UV emission line strength often correlate with the strength of Ciii]. We measured the velocity offsets of resonant emission lines with respect to systemic tracers as well as the electron density and the gas-phase abundance. Lastly, using "PhotoIonization Model Probability Density Functions" we find that the UV line emitters generally have ionization parameter log10(U) $\approx$ -2.5 and metal mass fractions that scatter around Z $\approx$ 10$^{-2}$, that is Z $\approx$ 0.66Z$\odot$. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper.
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MAGNUS III: Mild evolution of the total density slope in massive early-type galaxies since z$\sim$1 from dynamical modeling of MUSE integral-field stellar kinematics
University of California, Los Angeles（加州大学洛杉矶分校）；University of Oxford（牛津大学）；University of California, Davis（加州大学戴维斯分校）
Compact Core, Extended Reach: A Bipolar kpc-Scale Elongation in a Little Red Dot at $z \approx 5.5$
University of Arizona（亚利桑那大学）；University of Massachusetts Amherst（马萨诸塞大学阿默斯特分校）；NSF NOIRLab（美国国家光学-红外天文研究实验室）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；University of Cambridge（剑桥大学）
MUSE-DARK IV. Comparing Dark Matter Densities to Star Formation Histories in 375 intermediate-z galaxies
Université Lyon 1, ENS de Lyon, CNRS, CRAL（里昂第一大学，巴黎高等师范学院里昂分校，法国国家科学研究中心，里昂银河系与天体物理实验室）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；Univ. de Strasbourg, CNRS, Observatoire astronomique de Strasbourg（斯特拉斯堡大学，法国国家科学研究中心，斯特拉斯堡天文台）；Institute of Cosmology & Gravitation, University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）
