BUDHIES - III: the fate of H I and the quenching of galaxies in evolving environments
BUDHIES - III: the fate of H I and the quenching of galaxies in evolving environments
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DOI：
10.1093/mnras/stw984
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发表时间：
2016-04
影响因子：
4.8
通讯作者：
Y. Jaff'e;M. Verheijen;C. Haines;H. Yoon;R. Cybulski;M. Montero-Castano;Rory J. E. Smith;A. Chung;B. Deshev;Ximena Fern'andez;J. Gorkom;B. Poggianti;M. Yun;A. Finoguenov;Graham P. Smith;N. Okabe
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作者：
Y. Jaff'e;M. Verheijen;C. Haines;H. Yoon;R. Cybulski;M. Montero-Castano;Rory J. E. Smith;A. Chung;B. Deshev;Ximena Fern'andez;J. Gorkom;B. Poggianti;M. Yun;A. Finoguenov;Graham P. Smith;N. Okabe
在一个分层的宇宙中，星系团通过星系的吸积从场、群甚至其他星系团中成长。当这种情况发生时，星系可能会通过不同的机制失去和/或消耗它们的气体库，最终淬灭它们的星星形成。我们探索不同的环境历史的星系通过多波长的研究的综合效应的冲压压力剥离和组“处理”在阿贝尔963，一个巨大的增长集群z = 0.2从盲目超深H I环境调查（BUDHIES）。我们结合了数百个新的光学红移（总共有566个星团成员），以及来自LoCuSS的Subaru和XMM-牛顿数据，以确定子结构并评估星系形态，星星形成活动和H I含量（通过H I缺陷和堆叠）到3 × R200。我们发现，阿贝尔963是由至少七个集团，有助于大量的被动星系外的集群核心。更大质量的星系团有更高比例的被动和缺乏H I的星系，而低质量的星系团则拥有更年轻的（通常是相互作用的）星系。对于星系团星系不相关的群体，我们证实了我们以前的发现，H I气体（如果有的话）是显着剥离通过冲压压力在其第一次通过团内介质，并找到温和的证据与此事件相关的星爆。此外，我们发现了一个过剩的形态奇特和/或恒星形成星系附近的星系团的核心。我们推测，这些产生的影响，通过集群（后处理）的群体。我们的研究强调了环境淬火的重要性和不断变化的环境所增加的复杂性。
In a hierarchical Universe clusters grow via the accretion of galaxies from the field, groups and even other clusters. As this happens, galaxies can lose and/or consume their gas reservoirs via different mechanisms, eventually quenching their star formation. We explore the diverse environmental histories of galaxies through a multiwavelength study of the combined effect of ram-pressure stripping and group `processing' in Abell 963, a massive growing cluster at z = 0.2 from the Blind Ultra Deep H I Environmental Survey (BUDHIES). We incorporate hundreds of new optical redshifts (giving a total of 566 cluster members), as well as Subaru and XMM-Newton data from LoCuSS, to identify substructures and evaluate galaxy morphology, star formation activity, and H I content (via H I deficiencies and stacking) out to 3 × R200. We find that Abell 963 is being fed by at least seven groups, that contribute to the large number of passive galaxies outside the cluster core. More massive groups have a higher fraction of passive and H I-poor galaxies, while low-mass groups host younger (often interacting) galaxies. For cluster galaxies not associated with groups we corroborate our previous finding that H I gas (if any) is significantly stripped via ram-pressure during their first passage through the intracluster medium, and find mild evidence for a starburst associated with this event. In addition, we find an overabundance of morphologically peculiar and/or star-forming galaxies near the cluster core. We speculate that these arise from the effect of groups passing through the cluster (post-processing). Our study highlights the importance of environmental quenching and the complexity added by evolving environments.