Discovery of molecular gas fueling galaxy growth in a protocluster at z=1.7
Q. D'Amato, R. Gilli, I. Prandoni, C. Vignali, M. Massardi, M. Mignoli, O. Cucciati, T. Morishita, R. Decarli, M. Brusa, F. Calura, B. Balmaverde, M. Chiaberge,… 展开作者
Q. D'Amato, R. Gilli, I. Prandoni, C. Vignali, M. Massardi, M. Mignoli, O. Cucciati, T. Morishita, R. Decarli, M. Brusa, F. Calura, B. Balmaverde, M. Chiaberge, E. Liuzzo, R. Nanni, A. Peca, A. Pensabene, P. Tozzi, C. Norman
备注：
7 pages, 4 figures, 2 tables. Accepted for publication as a Letter in A&A
基于ALMA波段3对CO（2 - 1）线跃迁的观测，我们报道了在z = 1.7的过密区发现的三个新的富气星系（M_H2~1.5 - 4.8 × 10^10 M_sun，SFR范围~5 - 100 M_sun/yr），其中已经包含了八个光谱确认的成员。这导致了总共11个被确认的高密度成员，在投影距离约1.15 Mpc和红移范围Dz = 0.012内。在简单的假设下，我们估计该系统的总质量为>= 3 - 6 x 10^13 M_sun，并表明它可能在z = 0时演化为>~10^14 M_sun的星团。超密度包括一个强大的康普顿厚度的Fanaroff-Riley II型（FRII）射电星系，我们在其周围发现了一个大型分子气体库（M_H2~2 x 10^11 M_sun）。我们用长（短）轴为~27（~17）kpc的2-D高斯模型拟合FRII分辨的CO发射，这比光学静止框架发射大~3倍。在一个简单的边缘盘形态的假设下，我们发现星系星际介质产生了一个朝向核的柱密度，约为5.5 x 10^23 cm ^-2。这样一个致密的ISM可能会对X射线中测量到的总核遮蔽（N_（H，X）~1.5 x 10^24 cm ^-2）产生显著的影响，此外，中心引擎周围还有一个pc尺度的小吸收体。这个源的速度图揭示了垂直于无线电射流的气体旋转运动。FRII位于结构成员的投影空间分布的中心，其速度从红移分布的峰值偏移是在结构的速度色散范围内。所有这些，再加上FRII周围大量的气体，它的恒星质量约为3 × 10^11太阳质量，SFR约为200 - 600太阳质量/年，以及强大的射电-X射线辐射，表明这个源很可能是未来最明亮的星团星系的祖先。
英文摘要：
Based on ALMA Band 3 observations of the CO(2-1) line transition, we report the discovery of three new gas-rich (M_H2 ~ 1.5-4.8 x 10^10 M_sun, SFRs in the range ~5-100 M_sun/yr) galaxies in an overdense region at z=1.7, that already contains eight spectroscopically confirmed members. This leads to a total of 11 confirmed overdensity members, within a projected distance of ~ 1.15 Mpc and in a redshift range of Dz = 0.012. Under simple assumptions, we estimate that the system has a total mass of >= 3-6 x 10^13 M_sun, and show that it will likely evolve into a >~ 10^14 M_sun cluster at z = 0. The overdensity includes a powerful Compton-thick Fanaroff-Riley type II (FRII) radio-galaxy, around which we discovered a large molecular gas reservoir (M_H2 ~ 2 x 10^11 M_sun). We fitted the FRII resolved CO emission with a 2-D Gaussian model with major (minor) axis of ~ 27 (~ 17) kpc, that is a factor of ~3 larger than the optical rest-frame emission. Under the assumption of a simple edge-on disk morphology, we find that the galaxy interstellar medium produces a column density towards the nucleus of ~ 5.5 x 10^23 cm^-2. Such a dense ISM may then contribute significantly to the total nuclear obscuration measured in the X-rays (N_(H,X) ~ 1.5 x 10^24 cm^-2) in addition to a small, pc-scale absorber around the central engine. The velocity map of this source unveils a rotational motion of the gas that is perpendicular to the radio-jets. The FRII is located at the center of the projected spatial distribution of the structure members, and its velocity offset from the peak of the redshift distribution is well within the structure's velocity dispersion. All this, coupled with the large amount of gas around the FRII, its stellar mass of ~ 3 x 10^11 M_sun, SFR of ~ 200-600 M_sun/yr, and powerful radio-to-X-ray emission, suggests that this source is the likely progenitor of the future brightest cluster galaxy.
Fueling and feedback mechanisms at the nodes of the cosmic web
INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano（意大利国家天体物理研究所米兰空间天体物理与宇宙物理研究所）；INAF - Astronomical Observatory of Trieste（意大利国家天体物理研究所的里雅斯特天文台）；Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；INAF-Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切尔奇天文台）
Discovery of a $z\simeq 4.9$ Lyman-$α$ Emitter Protocluster: Wavelength-Dependent Environmental Effects on Galaxy Structure
National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies（日本综合研究大学院大学）；The University of Tokyo（东京大学）；Tohoku University（东北大学）
PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
School of Earth & Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Department of Astronomy/Steward Observatory, University of Arizona（亚利桑那大学天文系/斯图尔德天文台）；Joint ALMA Observatory（ALMA联合天文台）；National Astronomical Observatory of Japan（日本国立天文台）；European Southern Observatory（欧洲南方天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文系）；National Radio Astronomy Observatory（美国国家射电天文台）
A Possible Protocluster of Galaxies Serendipitously Discovered in the Field of an Intermediate-Redshift Post-starburst Galaxy
Texas A&M University（德州农工大学）；University of Pittsburgh（匹兹堡大学）；Rochester Institute of Technology（罗切斯特理工学院）；Princeton University（普林斯顿大学）；University of Colorado, Boulder（科罗拉多大学博尔德分校）
Early Emergence of Environmental Effects: Accelerated Galaxy Assembly in a z=2.96 Protocluster in the COSMOS Field
Tsinghua University（清华大学）；The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI)（宇宙物理与数学研究所（ Kavli IPMU ））
Strong environmental AGN enhancement among DSFGs in z > 2 protoclusters
University of Bologna（博洛尼亚大学）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所-天文与空间科学观测站）；Department of Physics and Astronomy, University of California, Davis（加州大学戴维斯分校物理与天文学系）；IFPU – Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Scuola Internazionale Superiore Studi Avanzati (SISSA)（国际高等研究院）；Gemini Observatory, NSF NOIRLab（吉米尼天文台，美国国家光学红外天文研究实验室）；Argelander-Institut für Astronomie, Univers（阿根德纳天文学研究所，大学）
Discovery of a Compact Hub-Filament System in G286.21+0.17 with JWST and ALMA: Insights into Protocluster Formation and Competitive Accretion
Peking University（北京大学）；National Astronomical Research Institute of Thailand（泰国国家天文研究所）；Gifu University（岐阜大学）；Indian Institute of Technology Gandhinagar（甘地纳加尔印度理工学院）；Korea Astronomy and Space Science Institute（韩国天文学与宇宙科学研究所）；University of Science and Technology, Korea (UST)（韩国科学技术院）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Nazarbayev University（纳扎尔巴耶夫大学）
Identifying a protocluster formation at z $\sim$ 4.5 in the COSMOS field: an extension of Taralay protocluster, traced by Ly-alpha emitters surrounding a submm galaxy
H I Absorbers as Beacons of Hidden Structure at $z \sim 3$: Multi-Component, Metal-Rich Absorption System near a Protocluster
The University of Tokyo（东京大学）；Shinshu University（信州大学）；Tohoku University（东北大学）；Hosei University（法政大学）；National Astronomical Observatory of Japan（日本国立天文台）
A cosmic collision in the making: JWST/NIRISS reveals a merging and maturing protocluster core at z~3 around a red quasar
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut（海德堡大学天文学中心，天文计算研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Department of Physics, Rhodes College（罗德学院物理系）；Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University（约翰斯·霍普金斯大学彭博中心物理与天文学系）；Institute for Advanced Study（高等研究院）；Department of Astronomy and Joint Space-Science Institute, University of Maryland, College Park（马里兰大学帕克分校天文学系及联合空间科学研究所）；Departamento de Astronomia, Instituto de Física, Universidade Federal do Rio Grande do Sul（南里奥格兰德联邦大学物理研究所天文学系）
A nine-member protostellar system forming via filament fragmentation in the high mass protocluster NGC 6334-43
Scottish Universities Physics Alliance (SUPA), School of Physics and Astronomy, University of St Andrews（圣安德鲁斯大学物理与天文学学院）；National Radio Astronomy Observatory（国家射电天文台）；Massachusetts Institute of Technology（麻省理工学院）；Aberystwyth University（阿伯里斯特威斯大学）
