Tracing the evolution of the cool gas in CGM and IGM environments through Mg II absorption from redshift z=0.75 to z=1.65 using DESI-Y1 data
X. Wu, Z. Cai, T. -W. Lan, S. Zou, A. Anand, Biprateep Dey, Z. Li, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, S. Ferraro, J. E. F… 展开作者
X. Wu, Z. Cai, T. -W. Lan, S. Zou, A. Anand, Biprateep Dey, Z. Li, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, S. Ferraro, J. E. Forero-Romero, S. Gontcho A Gontcho, K. Honscheid, S. Juneau, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, J. A. Newman, F. Prada, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, M. Siudek, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
We present a measurement of the mean absorption of cool gas traced by Mg II (${λλ2796, 2803}$) around emission line galaxies (ELGs), spanning spatial scales from 20 kpc to 10 Mpc. The measurement is based on cross-matching the positions of about 2.5 million ELGs at $z = 0.75-1.65$ and the metal absorption in the spectra of 1.4 million background quasars with data provided by the Year 1 sample of the Dark Energy Spectroscopic Instrument (DESI). The ELGs are divided into two redshift intervals: $0.75 < z < 1.0$ and $1.0 < z < 1.65$. We find that the composite spectra constructed by stacking the ELG-QSO pairs show evolution with redshift, with $z>1$ having a systematically higher signal of Mg II absorption. Within 1 Mpc, the covering fraction of the cool gas at $z > 1$ is higher than that of $z < 1$. The enhancement becomes less apparent especially if the projected distance $r_{p}>$1 Mpc. Also, ELGs with higher stellar mass and star formation rate (SFR) yield higher clustering of Mg II absorbers at $z<1$. For $z>1$, the covering fractions with different SFRs show little difference. The higher Mg II absorption at higher redshift also supports the observations of higher star formation at cosmic noon. Besides, the profile of Mg II absorption reveals a change of slope on scales of about 1 Mpc, consistent with the expected transition from a dark matter halo-dominated environment to a regime where clustering is dominated by halo-halo correlations. We estimate the cool gas density profile and derive the metal abundance at different redshifts. The growth of metal abundance suggests an increased presence of cool gas in the intergalactic medium (IGM) towards higher redshifts.
On the importance of the IGM/CGM enrichment in determining chemical abundances during the first 600 Myr
Department of Physics and Astronomy, Sam Houston State University（萨姆休斯顿州立大学物理与天文学系）；Minnesota Institute for Astrophysics, University of Minnesota（明尼苏达大学明尼苏达天体物理研究所）
Disentangling the galactic and intergalactic components in 313 observed Lyman-alpha line profiles between redshift 0 and 5
Observatori Astronòmic de la Universitat de València（瓦伦西亚大学天文台）；Departament d’Astronomia i Astrofísica, Universitat de València（瓦伦西亚大学天文学与天体物理学系）；Universität Heidelberg（海德堡大学）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Tsinghua University（清华大学）；IFCA-CSIC/Universitat de València（坎塔布里亚物理研究所CSIC-瓦伦西亚大学联合单位）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）
The Cosmic Ultraviolet Baryon Survey (CUBS) IX: The enriched circumgalactic and intergalactic medium around star-forming field dwarf galaxies traced by O VI absorption
本文基于 CUBS 数据通过 O VI 吸收线研究恒星形成矮星系周围的 CGM/IGM，发现低质量系统在 z≲1 时能有效将大量金属保留在附近的星系周与星系际介质中。
Intergalactic Medium Tomography with the Sunburst Arc
Texas Christian University（德克萨斯基督教大学）；University of Texas at Austin（得克萨斯大学奥斯汀分校）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Kavli Institute for the Physics and Mathematics of the Universe (WIP)（宇宙物理与数学卡弗里研究所（WIP））；National Astronomical Observatory of Japan（日本国立天文台）；Stockholm University（斯德哥尔摩大学）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics（宇宙学物理卡弗里研究所）；University of Michigan（密歇根大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Auckland（奥克兰大学）；University of Cincinnati（辛辛那提大学）；University of Oslo（奥斯陆大学）；Goddard Space Flight Center（戈达德太空飞行中心）；Centre de Recherche Astrophysique de Lyon UMR5574（里昂天体物理研究中心）
Probing Large-scale Structure and the Multi-Phase IGM at the Cosmic Noon -- Insights from a Joint Survey with Euclid, CSST, JPCam, and JUST
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Observatório Nacional（国家天文台）；University of Michigan（密歇根大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences(UCAS)（中国科学院大学天文与空间科学学院）；Department of Astronomy, Tsinghua University（清华大学天文系）；Department of Physics, University of Milano-Bicocca（米兰比可卡大学物理系）；Shanghai Jiao Tong University（上海交通大学）
Galaxy Proximate Damped Lyman-Alpha Systems and HI Reionization Topology in TECHNICOLOR DAWN
New Mexico State University（新墨西哥州立大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心（DAWN））；Niels Bohr Institute, University of Copenhagen / DTU-Space Technical University of Denmark（哥本哈根大学尼尔斯·玻尔研究所/丹麦技术大学空间研究所）
A dense, metal-rich absorber driven by a heavily dust-obscured galaxy: The direct evidence of CGM enrichment at $z\sim7$
University of Toronto（多伦多大学）；Dunlap Institute for Astronomy and Astrophysics（邓普天文学与天体物理研究所）；University of Copenhagen（哥本哈根大学）；Niels Bohr Institute（尼尔斯·玻尔研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究学院）；Massachusetts Institute of Technology（麻省理工学院）
Detecting the IGM metal enrichment with the 2-point correlation function of the flux. Application to the UVES deep spectrum
Università di Trieste（的里雅斯特大学）；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）；IFPU – Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；INFN – National Institute for Nuclear Physics（意大利国家核物理研究所）
On the Origin of the Ly$α$ Damping Wing in Galaxies at $8\le z \le 10$: Explorations using the NINJA Simulations
Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的的里雅斯特天文台）；IUCAA（印度大学天体物理学与宇宙学中心）；School of Physical Sciences, National Institute of Science Education and Research（国家科学教育研究学院物理科学学院）；Homi Bhabha National Institute（霍米·巴巴国立研究所）
Simba: The average properties of the circumgalactic medium of $2 \leq z \leq 3$ quasars are determined primarily by stellar feedback
利用Simba宇宙流体动力学模拟软件包研究了反馈对$2 \leq z \leq 3$类星体周围环星系介质和星系际介质的影响。我们发现辛巴类星体是吸积速度最快的黑洞，并表明它们在热光度和相关强度上与真正的类星体很好地匹配。我们提取莱曼α（Ly-a）吸收光谱通过在不同的横向距离（10千秒差距$\lesssim b \lesssim$ 10百万秒差距）周围的类星体，并比较观察到的平均Ly-a吸收曲线。观测结果被很好地再现，除了在100 kpc的前景类星体，辛巴过度产生吸收;这可能会通过包括类星体本身的电离来减轻。通过比较不同的反馈模块激活的运行，我们发现，（机械）AGN反馈对周围的CGM几乎没有影响，即使在这些最高亮度的黑洞，而恒星反馈有显着的影响。通过进一步研究CGM气体的热力学和运动学性质，我们发现恒星反馈而不是活动星系核反馈是决定$z\sim 2-3$类星体周围CGM平均性质的主要物理驱动因素。我们还比较了我们的结果与以前的作品，并发现辛巴预测更多的吸收在100千秒差距内比尼克斯和Illustris模拟，表明Ly-a吸收曲线可以是一个强大的约束模拟。VLT-MUSE等工具和即将进行的调查（例如，WEAVE和DESI）承诺进一步改进此类约束。
Ardua: Unveiling the Baryon Cycle from Stars to the Cosmic Web
University of Arizona（亚利桑那大学）；NASA Goddard Space Flight Center（NASA戈达德太空飞行中心）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森天体物理中心）；New Mexico State University（新墨西哥州立大学）；Northwestern University（西北大学）；University of Colorado Boulder（科罗拉多大学博尔德分校）；University of Florida（佛罗里达大学）；University of South Carolina（南卡罗来纳大学）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）
EIGER VIII: First stars signatures in the connection between OI absorption and Galaxies in the Epoch of Reionization
North Carolina State University（北卡罗来纳州立大学）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究研究所）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究所）；National Astronomical Observatory of Japan (NAOJ)（日本国立天文台）；ETH Zürich（苏黎世联邦理工学院）
