Formation of globular cluster systems: from dwarf galaxies to giants
Formation of globular cluster systems: from dwarf galaxies to giants
复制标题
球状星团系统的形成：从矮星系到巨星系
DOI：
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发表时间：
2018
影响因子：
4.8
通讯作者：
Hui Li
中科院分区：
文献类型：
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作者：
Nick Choksi;O. Gnedin;Hui Li
球状星团（GC）系统周围的星系的巨大质量范围显示出非常简单的标度关系。所有GC的总质量是一个恒定的分数的总星系质量和GC系统的平均金属丰度和金属丰度分散度的规模与星系质量弱。大质量的贫金属（蓝色）星团的金属丰度随着星团质量的增加而增加，而富金属（红色）星团的金属丰度则不增加。一个显着的年龄-金属丰度关系出现在银河系GC和未解决的人口在附近星系的恒星种群解析。值得注意的是，所有这些趋势都可以解释一个简单的合并为基础的模型在以前的工作和更新在这里使用最近的观测星系标度关系在高红移。我们发现，GC金属丰度分布与星系质量的增加分散是一个强大的预测模型。它产生于更大质量的星系有更多的合并，结合联合收割机卫星GC系统。晕团的平均金属丰度比3 dex增加0.6 dex。模型显示GC系统质量和宿主星系质量之间存在非线性趋势，这与数据一致。该模型不考虑GC自富集，但预测的大规模蓝色集群的集群质量和金属丰度之间的相关性。年龄-金属丰度关系是该模型的另一个可靠预测。所有星系团中有一半预计将在红移范围内形成
Globular cluster (GC) systems around galaxies of a vast mass range show remarkably simple scaling relations. The combined mass of all GCs is a constant fraction of the total galaxy mass and the mean metallicity and metallicity dispersion of the GC system scale up weakly with galaxy mass. The metallicity of massive, metal-poor ("blue") clusters increases with cluster mass, while that of metal-rich ("red") clusters does not. A significant age-metallicity relation emerges from analysis of resolved stellar populations in Galactic GCs and unresolved populations in nearby galaxies. Remarkably, all these trends can be explained by a simple merger-based model developed in previous work and updated here using recent observations of galaxy scaling relations at high redshift. We show that the increasing dispersion of GC metallicity distributions with galaxy mass is a robust prediction of the model. It arises from more massive galaxies having more mergers that combine satellite GC systems. The average metallicity also increases by 0.6~dex over 3~dex in halo mass. The models show a non-linear trend between the GC system mass and host galaxy mass which is consistent with the data. The model does not consider GC self-enrichment, yet predicts a correlation between cluster mass and metallicity for massive blue clusters. The age-metallicity relation is another robust prediction of the model. Half of all clusters are predicted to form within the redshift range $5
影响因子：
64.8
作者：
M. Vogelsberger;S. Genel;V. Springel;P. Torrey;D. Sijacki;Da Xu;G. Snyder;Simeon Bird;D. Nelson;Lars Hernquist Mit;HarvardCfA;Hits;I. Cambridge;Stsci;Ias Princeton
通讯作者：
M. Vogelsberger;S. Genel;V. Springel;P. Torrey;D. Sijacki;Da Xu;G. Snyder;Simeon Bird;D. Nelson;Lars Hernquist Mit;HarvardCfA;Hits;I. Cambridge;Stsci;Ias Princeton
DOI：
10.1088/0004-637x/739/1/45
发表时间：
2011-04
期刊：
The Astrophysical Journal
影响因子：
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作者：
N. F. Schreiber;A. Shapley;R. Genzel;N. Bouché;G. Cresci;R. Davies;D. Erb;S. Genel;D. Lutz
通讯作者：
N. F. Schreiber;A. Shapley;R. Genzel;N. Bouché;G. Cresci;R. Davies;D. Erb;S. Genel;D. Lutz
为 JWST 铺平道路：见证 z > 3 处球状星团的形成
影响因子：
4.8
作者：
Vanzella;Calura;Meneghetti;Mercurio;Castellano;Caminha;Balestra;Rosati;De Barros;Grazian;D'Ercole;Ciotti;Caputi;Grillo;Merlin;Pentericci;Fontana;Cristiani
通讯作者：
Cristiani