Formation histories of stars, clusters, and globular clusters in the E-MOSAICS simulations
Formation histories of stars, clusters, and globular clusters in the E-MOSAICS simulations
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E-MOSAICS 模拟中恒星、星团和球状星团的形成历史
DOI：
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发表时间：
2019
影响因子：
4.8
通讯作者：
R. Crain
中科院分区：
文献类型：
--
作者：
M. Reina;J. Kruijssen;J. Pfeffer;N. Bastian;R. Crain
球状星团（GCs）的形成历史是理解它们与宇宙时间演化关系的关键诊断。我们使用来自e - mosaic项目的25个现代银河系质量星系的宇宙学放大模拟来研究恒星，星团和gc的形成历史，以及它们如何受到星团形成物理的环境依赖性的影响。我们发现这些星系中GC形成的中位回溯时间为${\sim}10.73~$ Gyr ($z=2.1$)，大约比野星（${\sim}8.34~$ Gyr或$z=1.1$）早$2.5~$ Gyr。气相色谱峰形成的时代主要由最大星团质量的时间演化决定，这取决于星系环境，并在很大程度上随气体压力的增加而增加。不同金属丰度的恒星、星团和gc呈现重叠的形成历史，表明恒星和星团的形成过程是连续的。我们星系中缺乏金属的GC （$-2.5<[\rm Fe/H]<-1.5$）比富含金属的GC亚群（$-1.0<[\rm Fe/H]<-0.5$）更古老，分别形成$12.13~$ Gyr和$10.15~$ Gyr ago （$z=3.7$和$z=1.8$）。GC的中位年龄随着金属丰度的增加而逐渐减小，说明不同GC金属丰度亚群不是独立形成的，其空间和运动分布是在分层星系形成演化背景下演化的结果。我们预测原始gc的形成在$2\lesssim z \lesssim 3$最普遍，这可以通过使用JWST对透镜星系的观测来验证。
The formation histories of globular clusters (GCs) are a key diagnostic for understanding their relation to the evolution of the Universe through cosmic time. We use the suite of 25 cosmological zoom-in simulations of present-day Milky Way-mass galaxies from the E-MOSAICS project to study the formation histories of stars, clusters, and GCs, and how these are affected by the environmental dependence of the cluster formation physics. We find that the median lookback time of GC formation in these galaxies is ${\sim}10.73~$Gyr ($z=2.1$), roughly $2.5~$Gyr earlier than that of the field stars (${\sim}8.34~$Gyr or $z=1.1$). The epoch of peak GC formation is mainly determined by the time evolution of the maximum cluster mass, which depends on the galactic environment and largely increases with the gas pressure. Different metallicity subpopulations of stars, clusters and GCs present overlapping formation histories, implying that star and cluster formation represent continuous processes. The metal-poor GCs ($-2.5<[\rm Fe/H]<-1.5$) of our galaxies are older than the metal-rich GC subpopulation ($-1.0<[\rm Fe/H]<-0.5$), forming $12.13~$Gyr and $10.15~$Gyr ago ($z=3.7$ and $z=1.8$), respectively. The median ages of GCs are found to decrease gradually with increasing metallicity, which suggests different GC metallicity subpopulations do not form independently and their spatial and kinematic distributions are the result of their evolution in the context of hierarchical galaxy formation and evolution. We predict that proto-GC formation is most prevalent at $2\lesssim z \lesssim 3$, which could be tested with observations of lensed galaxies using JWST.
DOI：
10.1111/j.1365-2966.2009.15034.x
发表时间：
2008-08
影响因子：
4.8
作者：
K. Dolag;S. Borgani;S. Borgani;S. Borgani;G. Murante;V. Springel
通讯作者：
K. Dolag;S. Borgani;S. Borgani;S. Borgani;G. Murante;V. Springel
分子云、星团和高红移团块最大质量尺度的统一模型
影响因子：
4.8
作者：
Reina-Campos;Kruijssen
通讯作者：
Kruijssen