The Local Cluster Survey II: disc-dominated cluster galaxies with suppressed star formation
The Local Cluster Survey II: disc-dominated cluster galaxies with suppressed star formation
复制标题
本地星团巡天 II：恒星形成受到抑制的盘主导星团星系
DOI：
10.1093/mnras/stad640
复制
发表时间：
2023
影响因子：
4.8
通讯作者：
Zaritsky, Dennis
中科院分区：
文献类型：
--
作者：
Finn, Rose A.;Vulcani, Benedetta;Rudnick, Gregory;Balogh, Michael L.;Desai, Vandana;Jablonka, Pascale;Zaritsky, Dennis
我们通过研究来自本地星团调查（0.0137 <z< 0.0433）的9个星团中的恒星形成星系和来自斯隆数字巡天的大型比较场样本，研究了密集环境在抑制恒星形成中的作用。我们比较了恒星形成速率（SFR）与恒星质量关系作为环境和形态的函数。在仔细控制质量后，我们发现在所有环境中，SFR抑制程度都随着凸起-总（B/T）比的增加而增加。此外，在所有b /T值下，固定质量的星系团和落入星系的SFRs比它们的场对应物受到更大的抑制。这些结果表明，在所有环境中都存在一种与凸起生长有关的猝灭机制，以及一种进一步降低致密环境中星系SFRs的附加机制。我们将样本限制在b /T≤0.3的星系，以控制形态学的趋势，并发现具有抑制SFRs的星系团星系的过剩人口仍然存在。我们对致密环境中与SFRs下降相关的时间尺度进行了建模，发现观测到的星系团核心星系的SFRs与一系列模型一致，包括在长（2-5 Gyr）时间尺度上缓慢而连续地起作用的机制，以及在1 - 6 Gyr延迟期后发生的更快速（<1 Gyr）猝灭事件。因此，猝灭可能在星系进入星系团后立即开始。
We investigate the role of dense environments in suppressing star formation by studyingstar-forming galaxies in nine clusters from theLocal Cluster Survey(0.0137 <z< 0.0433) and a large comparison field sample drawn from the Sloan Digital Sky Survey. We compare the star formation rate (SFR) with stellar mass relation as a function of environment and morphology. After carefully controlling for mass, we find that in all environments, the degree of SFR suppression increases with increasing bulge-to-total (B/T) ratio. In addition, the SFRs of cluster and infall galaxies at a fixed mass are more suppressed than their field counterparts at all values ofB/T. These results suggest a quenching mechanism that is linked to bulge growth that operates in all environments and an additional mechanism that further reduces the SFRs of galaxies in dense environments. We limit the sample toB/T≤ 0.3 galaxies to control for the trends with morphology and find that the excess population of cluster galaxies with suppressed SFRs persists. We model the time-scale associated with the decline of SFRs in dense environments and find that the observed SFRs of the cluster core galaxies are consistent with a range of models including a mechanism that acts slowly and continuously over a long (2–5 Gyr) time-scale, and a more rapid (<1 Gyr) quenching event that occurs after a delay period of 1–6 Gyr. Quenching may therefore start immediately after galaxies enter clusters.