大质量红星系的形成：耶鲁-智利多波长巡天（MUSYC）中z <2的色星等和色恒星质量图
The Rise of Massive Red Galaxies: the color-magnitude and color-stellar mass diagrams for z < ~2 from the MUltiwavelength Survey by Yale-Chile (MUSYC)
摘要：
基于耶鲁-智利多波长巡天（MUSYC）的扩展Chandra深场南（ECDFS）星表K < 22（AB），给出了z_phot <2星系的色星等图和色恒星质量图。我们的7840个星系的主要样本包含1297个M_* > 10^11 M_Sol星系，范围为0.2 < z_phot < 1.8。我们的经验表明，对于z_phot < 1.8的M_* > 10^11 M_Sol星系，这个星表是近似完整的。对于这个质量有限的样本，我们证明了红序色-恒星质量关系的轨迹是：当z_phot < ~1.2时，Del（u-r）~（-0.44+/-0.02）z_phot。然而，对于z_phot > ~1.3，我们不再能够从观察到的颜色分布中可靠地区分红色和蓝色亚群;我们表明，这将需要更深的近红外数据。在1.5 < z_phot <1.8时，M_* > 10^11 M_Sol星系的共动数密度约为局域值的50%，红色部分约为33%。对观测到的演化进行参数拟合，我们发现n_tot（z）~（1+z_phot）^（-0.52+/-0.12（+/-0.20））。我们发现红色部分的演化更强：f_red（z）~（1+z_phot）^（-1.17+/-0.18（+/-0.21））。通过一系列的灵敏度分析，我们表明，最重要的系统误差的来源是：1。z~0和z>>0样本分析的系统性差异; 2.与光度红移计算的细节相关的系统效应;以及3.光度校准中的不确定性。考虑到这一点，我们表明，我们的光度红移的基础上的结果是一致的一个完全独立的分析，不需要红移信息的个别星系。我们的结果表明，最多有1/5的M_* >10^11 M_Sol的局域红序星系在z ~ 2时已经就位。
英文摘要：
We present the color-magnitude and color-stellar mass diagrams for galaxies with z_phot < ~2, based on a K < 22 (AB) catalog of the Extended Chandra Deep Field South (ECDFS) from the MUltiwavelength Survey by Yale-Chile (MUSYC). Our main sample of 7840 galaxies contains 1297 M_* > 10^11 M_Sol galaxies in the range 0.2 < z_phot < 1.8. We show empirically that this catalog is approximately complete for M_* > 10^11 M_Sol galaxies for z_phot < 1.8. For this mass-limited sample, we show that the locus of the red sequence color-stellar mass relation evolves as Del(u-r) ~ (-0.44+/-0.02) z_phot for z_phot < ~1.2. For z_phot > ~1.3, however, we are no longer able to reliably distinguish red and blue subpopulations from the observed color distribution; we show that this would require much deeper near infrared data. At 1.5 < z_phot <1.8, the comoving number density of M_* > 10^11 M_Sol galaxies is ~50% of the local value, with a red fraction of ~33%. Making a parametric fit to the observed evolution, we find n_tot(z) ~ (1+z_phot)^(-0.52+/-0.12(+/-0.20)). We find stronger evolution in the red fraction: f_red(z) ~ (1+z_phot)^(-1.17+/-0.18(+/-0.21)). Through a series of sensitivity analyses, we show that the most important sources of systematic error are: 1. systematic differences in the analysis of the z~0 and z>>0 samples; 2. systematic effects associated with details of the photometric redshift calculation; and 3. uncertainties in the photometric calibration. With this in mind, we show that our results based on photometric redshifts are consistent with a completely independent analysis which does not require redshift information for individual galaxies. Our results suggest that, at most, 1/5 of local red sequence galaxies with M_* >10^11 M_Sol were already in place at z ~ 2.
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