Environmental effects at early cosmic times: galaxy evolution in the first massive clusters

早期宇宙时代的环境影响：第一个巨大星团中的星系演化

• 批准号: 394232321
• 负责人: Professor Dr. Joseph Mohr, since 12/2019
• 金额: --
• 依托单位: Max-Planck-Institut für extraterrestrische Physik (MPE)
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2018
• 资助国家: 德国
• 起止时间: 2017-12-31 至 2020-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/394232321?language=en
• 关键词: Environmental; effects; early; cosmic; times

This project is based on recently obtained, deep, homogeneous imaging follow-up with HST and Spitzer of the complete sample of five high-significance (S/N>5) galaxy clusters at z>~1.4 detected through the Sunyaev-Zeldovich effect in the SPT-SZ survey over 2500 square degrees. The large survey area and depth of SPT-SZ allow the identification of this still unique sample of clusters among the rarest, most massive known at this cosmic epoch. The cluster selection, tightly related to cluster mass and totally independent of cluster galaxies (unlike most cluster surveys at these redshifts), makes this sample uniquely suited for unbiased galaxy population studies probing environmental signatures on galaxy evolution in early cluster environments. We designed the specific combination of HST and Spitzer observations to provide a first "essential data set" to start efficiently probing galaxy populations in terms of star formation and quenching, stellar mass assembly, passive fractions vs. stellar mass, formation of the red sequence, formation and evolution of Brightest Cluster Galaxies, morphologies vs. stellar population properties, structural evolution of bulge- and disk-dominated galaxies, and merger rates and properties in these extreme environments, as well as the galaxy stellar mass function, halo occupation distribution and stellar mass fraction in most massive halos at z~1.5. All HST and Spitzer observations are now completed and reduced. First analyses are ongoing with a DLR-supported program focused on the HST observations, confirming the high-redshift nature of these clusters, with the most distant system being consistently estimated at z~1.8 from both the (totally independent) red-sequence and X-ray modeling analyses. At this redshift, it is not only the most distant cluster discovered in the SPT-SZ survey, but the most distant massive (M500>10^14 Msun) ICM-selected cluster discovered thus far, and potentially the most distant cluster known in this extreme mass range irrespective of selection. We ask here for support for continuing this work, in particular fully exploiting the synergy between HST and Spitzer observations which is critical to the goals of this investigation.The proposed project will allow us to complete the first study of this kind of such a well defined, homogeneous massive distant cluster sample, and exploit its pilot-project nature for an efficient design of follow-up of distant clusters for galaxy evolution studies for new and coming surveys (SPTpol, SPT-3G, eROSITA), bridging today's state-of-the-art work and its powerful future extensions.

该项目是基于最近获得的、使用HST和Spitzer对5个高显著性（S/N>5）星系团的完整样本进行的深度均匀成像跟踪，这些星系团在2500平方度的SPT-SZ巡天中通过Sunyaev-Zeldovich效应探测到z> 1.4。SPT-SZ的大调查区域和深度允许在这个宇宙时代已知的最稀有，最大的星团中识别这个仍然独特的样本。星系团的选择，密切相关的集群质量和完全独立的星系团星系（不像大多数集群调查在这些红移），使这个样本非常适合无偏见的星系人口研究探索环境的签名星系演化在早期的星系团环境。我们设计了HST和斯皮策观测的特定组合，以提供第一个“基本数据集”，开始有效地探测星系种群，包括星星的形成和淬灭，恒星质量组装，被动分数与恒星质量，红色序列的形成，Brilliant星团Galerkin的形成和演化，形态与恒星种群特性，隆起和盘主导星系的结构演化，和这些极端环境中的合并速率和性质，以及星系恒星质量函数，晕占据分布和恒星质量分数在大多数质量晕在z~1.5。 所有的HST和斯皮策观测现在都已经完成并缩小了。第一个分析正在进行中，DLR支持的程序专注于HST观测，证实了这些星系团的高红移性质，最遥远的系统一致地估计在z~1.8（完全独立的）红色序列和X射线建模分析。在这个红移下，它不仅是SPT-SZ巡天中发现的最遥远的星团，也是迄今为止发现的最遥远的大质量（M500>10^14 Msun）ICM选择星团，并且可能是在这个极端质量范围内已知的最遥远的星团。 我们在这里请求支持继续这项工作，特别是充分利用HST和斯皮策观测之间的协同作用，这对实现这项研究的目标至关重要。拟议的项目将使我们能够完成对这种定义良好的、均匀的大质量遥远星团样本的首次研究，并利用其试点项目的性质，为新的和即将到来的调查进行星系演化研究的遥远星系团的后续有效设计（SPTpol，SPT-3G，eROSITA），连接当今最先进的工作及其强大的未来扩展。

项目成果

Galaxy populations in the most distant SPT-SZ clusters

• DOI: 10.1051/0004-6361/201833944
• 发表时间: 2018-07
• 期刊: Astronomy & Astrophysics
• 影响因子: 6.5
• 作者: V. Strazzullo;M. Pannella;J. Mohr;A. Saro;M. Ashby;M. Bayliss;S. Bocquet;E. Bulbul;G. Khullar-G.-Khul