Spectroscopic observations of PHz G237.01+42.50: A galaxy protocluster at z=2.16 in the Cosmos field
M. Polletta, G. Soucail, H. Dole, M. D. Lehnert, E. Pointecouteau, G. Vietri, M. Scodeggio, L. Montier, Y. Koyama, G. Lagache, B. L. Frye, F. Cusano, M. Fumana
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(40 pages, 28 figures) Accepted for publication in A&A
The Planck satellite has identified more than 2000 protocluster candidates with extreme star formation rates (SFRs). Here, we present the spectroscopic identification of a Planck-selected protocluster located in the Cosmos field, PHz G237.01+42.50 (G237). G237 contains a galaxy overdensity of 31 spectroscopically identified galaxies at z~2.16 (significant at 5.4 sigma) in a 10'x11' region. The overdensity contains two substructures or protoclusters at <z>~2.16 and 2.195 with estimated halo masses at z=0 of ~(5-6)x10^14 Msun. The overdensity total SFR, ~4000 Msun/yr, is higher than predicted by simulations but much smaller than the SFR derived from the Planck data. The analysis of the Herschel data, in combination with the available ancillary data, shows that such a difference is due to an effect of source alignment along the line of sight that produces a 5 sigma overdensity of red Herschel sources in the field. We analyze the members' UV spectra and UV-far-infrared spectral energy distributions to derive their SFR, stellar mass, and metallicity. Galaxy members include blue star-forming galaxies and AGN with SFRs and stellar masses consistent with the main sequence. AGN, identified through optical spectroscopy or X-ray data, represent a significant fraction (20+/-10%) of all members of the protocluster at z=2.16, and they are powerful enough to produce radiative feedback. The core of this protocluster, besides being denser, includes members that are, on average, more massive and star-forming and contains a larger fraction of AGN and Herschel-detected galaxies than the full sample, suggesting an environmental effect on galaxy growth. A comparison between G237 and other protoclusters in the literature at similar redshifts reveals some common traits and differences that reflect both observational biases and a diversity in intrinsic properties that is not yet fully understood.
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
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 ））
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）
ODIN: Characterizing the Three-dimensional Structure of Two Protocluster Complexes at $z = 3.1$
Purdue University（普渡大学）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Universidad Andres Bello（安德烈斯贝略大学）；University College London（伦敦大学学院）
SILVERRUSH. VII. Subaru/HSC Identifications of 42 Protocluster Candidates at z~6-7 with the Spectroscopic Redshifts up to z=6.574: Implications for Cosmic Reionization
Diverse Metallicities in Protoclusters at $z \sim 3.4$ detected by Deep Learning
The University of Tokyo（东京大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心 (DAWN)）；Technical University of Denmark（丹麦技术大学）；University of Hyogo（兵库大学）；Tohoku University（东北大学）；Kwansei Gakuin University（关西学院大学）；Carnegie Institution for Science（卡内基科学机构）；National Astronomical Observatory of Japan（日本国立天文台）
The assembly and fate of a giant disc galaxy in a protocluster at $z = 3$
Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Leiden Observatory, Leiden University（莱顿大学莱登天文台）；Dipartimento di Fisica e Astronomia "Augusto Righi", Alma Mater Studiorum Università di Bologna（博洛尼亚大学物理与天文学系）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚空间科学与天体物理观测站）；INFN-Sezione di Bologna（博洛尼亚意大利国家核物理研究所）
Do Submillimeter Galaxies Trace Megaparsec Large-scale Structures? -- An Overdensity Analysis of 449 Submillimeter Galaxies in COSMOS
Purple Mountain Observatory, Chinese Academy of Science（中国科学院紫金山天文台）；School of Astronomy and Space Sciences, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）；State Key Laboratory of Radio Astronomy and Technology, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台射电天文与技术重点实验室）；Instituto de Astrofísica de Canarias (IAC)（加那利天体物理研究所）；Universidad de La Laguna（拉古纳大学）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间科学观测站）；INAF-Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Dipartimento di Fisica e Astronomia “A. Righi”, Alma Mater Studiorum Università di Bologna（博洛尼亚大学阿玛·玛特·斯图迪奥鲁姆物理与天文学“A. Righi”系）
The 700 ks Chandra Spiderweb Field I: evidence for widespread nuclear activity in the Protocluster
(Abridged) We present an analysis of the 700 ks Chandra ACIS-S observation of the field around the Spiderweb Galaxy at z=2.156, focusing on the nuclear activity in the associated large-scale environment. We identify unresolved X-ray sources down to flux limits of 1.3X10^{-16} and 3.9X10^{-16} erg/s/cm^2 in the soft and hard band, respectively. We search for counterparts in the optical, NIR and submm bands to identify X-ray sources belonging to the protocluster. We detect 107 X-ray unresolved sources within 5 arcmin (corresponding to 2.5 Mpc) of J1140-2629, among which 13 have optical counterpa…
ODIN: Confirmation and 3D Reconstruction of Six Massive Protoclusters at Cosmic Noon
Purdue University（普渡大学）；NSF NOIRLab（美国国家光学-红外天文研究实验室）；Arizona State University（亚利桑那州立大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Boston University（波士顿大学）；Universidad Andres Bello（安德烈斯贝略大学）；Università degli Studi di Milano（米兰大学）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
A Search for Massive Galaxy Population in a Protocluster of LAEs at $z = 2.39$ near the Radio Galaxy 53W002
利用Subaru望远镜Suprime-Cam和MOIRCS的$B,~V,~i^\prime,~J,~H,~{\rm{and}}~K_s$波段成像数据，在射电星系53 W 002附近的$z=2.39$观测到的莱曼$~α$发射体（LAEs）的已知大尺度高密度结构中寻找大质量星系群。在我们的巡天$70.2~{\rm{arcmin}}^{2}$中，我们通过$JHK_s$波段颜色和光谱能量分布（SED）拟合分析（$JHK_s$ -selected galaxies）选择了62个原星系候选成员，并将它们的物理性质与COSMOS场中的一个比较样本进行了比较。我们发现在$K_s<22.25,~J-K_s>2,~{\rm{or}}~V-K_s>4$的53 W 002场中，$JHK_s$选择星系的数密度显著过剩。特别是在53 W 002视场中具有$K_s<22.25~{\rm{and}}~J-K_s>2$的$JHK_s$选定星系的数密度比比较样本高9倍。大多数具有$K_s<22.25~{\rm{and}}~J-K_s>2$的星系都是具有$M_s>10^{11}~M_\odot$的大质量星系，它们的sSFR为$10^{-11}$ -- $10^{-10}~\rm{yr^{-1}}$，表明恒星形成尚未完全停止。我们还发现了具有$M_s=5\times10^{10}$ -$10^{11}~M_\odot~{…
