The Red Sequence of High-Redshift Clusters: A Comparison with Cosmological Galaxy Formation Models
The Red Sequence of High-Redshift Clusters: A Comparison with Cosmological Galaxy Formation Models
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DOI：
10.1086/591016
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发表时间：
2008-06
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通讯作者：
N. Menci;P. Rosati;R. Gobat;V. Strazzullo;A. Rettura;S. Mei;R. D. Inaf;Osserv. Astronomico di Roma European Southern Observatory-Osserv.-Astronomico-di-Roma-European-Southern-2291069956;2. Karl-Schwarzschild-Strasse;Garching;Germany National Radio Astronomy Observatory;Socorro;Nm;USA. Department of physics;Astronomy;John s Hopkins University;Baltimore;Md;Usa University of Paris Denis Diderot;Paris Cédex;France Paris;S. Meudon;Meudon Cedex;France
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作者：
N. Menci;P. Rosati;R. Gobat;V. Strazzullo;A. Rettura;S. Mei;R. D. Inaf;Osserv. Astronomico di Roma European Southern Observatory-Osserv.-Astronomico-di-Roma-European-Southern-2291069956;2. Karl-Schwarzschild-Strasse;Garching;Germany National Radio Astronomy Observatory;Socorro;Nm;USA. Department of physics;Astronomy;John s Hopkins University;Baltimore;Md;Usa University of Paris Denis Diderot;Paris Cédex;France Paris;S. Meudon;Meudon Cedex;France
我们将最先进的星系形成半解析模型的结果与在0.8≤z≤1.3范围内观测到的遥远星系团的分光光度观测结果进行了比较。我们研究了它们的红序列（RS）星系的性质，并将它们与相同红移的场进行了比较。在我们的模型中，我们发现(1)通过z≈1.2已经得到了一个定义良好的窄RS；这被发现比场RS更密集，类似于在z = 0时观察和预测的情况；(2)在z = 1.2时，聚类RS预测的U-V休息帧颜色和散度的平均值分别为1和0.15，聚类间方差分别为≈0.2和≈0.06。星系团的RS散射比相应的场值小约5倍；(3)考虑RS星系时，z≈1.2时场星系和星系团星系的质量增长历史相似，z = 1.2时RS星系90%的恒星质量在宇宙时间t = 2.5 Gyr时已经形成，t = 1 Gyr时50%的恒星质量已经形成；(4)星团群和野群在z = 1.2处的恒星年龄预测分布（峰值为3.7 Gyr）；然而，对于后者，分布明显向较低年龄倾斜。虽然在z≈1.2处观测到的聚类RS散射的平均值ΔU−V≈0.07小于相应的模型中心值，但与观测值相比，上述结果总体上是一致的。我们在宇宙星系形成的框架内讨论了上述结果的物理起源和意义。
We compare the results from a state-of-the-art semianalytic model of galaxy formation with spectrophotometric observations of distant galaxy clusters observed in the range 0.8 ⩽ z⩽ 1.3. We investigate the properties of their red sequence (RS) galaxies and compare them with those of the field at the same redshift. In our model we find that (1) a well-defined, narrow RS is obtained already by z ≈ 1.2; this is found to be more populated than the field RS, analogously to what is observed and predicted at z = 0; (2) the predicted U–V rest-frame colors and scatter of the cluster RS at z = 1.2 have average values of 1 and 0.15, respectively, with a cluster-to-cluster variance of ≈0.2 and ≈0.06, respectively. The scatter of the RS of cluster galaxies is ≈5 times smaller than the corresponding field value; (3) when the RS galaxies are considered, the mass growth histories of field and cluster galaxies at z ≈ 1.2 are similar, with 90% of the stellar mass of RS galaxies at z = 1.2 already formed at cosmic times t = 2.5 Gyr, and 50% at t = 1 Gyr; and (4) the predicted distribution of stellar ages of RS galaxies at z = 1.2 peaks at 3.7 Gyr for both cluster and field populations; however, for the latter the distribution is significantly skewed toward lower ages. When compared with observations, the above findings show an overall consistency, although the average value ΔU − V ≈ 0.07 of the observed cluster RS scatter at z ≈ 1.2 is smaller than the corresponding model central value. We discuss the physical origin and the significance of the above results in the framework of cosmological galaxy formation.