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首页> 外文期刊>The Astrophysical journal >THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY: THE MORPHOLOGY-DENSITY RELATION OF GALAXIES OUT TO z ～ 1~1
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THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY: THE MORPHOLOGY-DENSITY RELATION OF GALAXIES OUT TO z ～ 1~1

机译：加拿大-法国-夏威夷遥测的遗产调查：z〜1〜1范围内星系的形态密度关系

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摘要

We study the relationships between galaxy total luminosity (M_(g′)), morphology, color, and environment as a function of redshift. We use a magnitude-limited sample of 65,624 galaxies in the redshift range 0 < z < 1.3 taken from one of the 1° x 1° Canada-France-Hawaii Telescope Legacy Survey Deep Fields. We parameterize galaxy morphology according to the Sersic index n, taking n > 2 to be "bulge-dominated" and n < 2 to be "disk-dominated." Our n > 2 number fractions at z = 0.1 agree well with those based on Sloan Digital Sky Survey galaxies. We find that the n > 2 galaxy number fraction is constant with redshift in the field. However, for overdense environments, this fraction is larger and increases toward lower redshifts, higher densities, and higher luminosities. Rest-frame color-magnitude diagrams show that the color distribution is bimodal out to our redshift limit of z ～ 1, with a prominent red sequence of galaxies at 0.2 < z < 0.4 and a large blue-peak dominance at 0.8 < z < 1. We use this bimodality to define a red fraction as the fraction of galaxies having a rest-frame color u~* - g′ > 1. For all environments, this fraction increases toward lower redshifts and higher luminosities. The red fraction within cluster-like regions changes 60% faster with redshift as compared to the field for galaxies with M_(g′) < -19.5. Using, for the first time, observations across many cluster-field interfaces distributed over a single, large volume, we trace the large-scale morphology-density relation and the Butcher-Oemler effect over a period of almost 8 Gyr.
机译：我们研究了银河系总亮度（M_（g'）），形态，颜色和环境之间的关系，这些关系是红移的函数。我们使用从1°x 1°加拿大-法国-夏威夷望远镜遗留测量深场之一获取的红移范围0 2为“凸起为主”，n <2为“磁盘为主”。我们在z = 0.1时的n> 2个数字分数与基于斯隆数字天空测量星系的数字分数非常吻合。我们发现，n> 2的星系数分数在场中随红移而恒定。但是，对于密度过大的环境，此分数更大，并且向着较低的红移，较高的密度和较高的发光度增加。静止帧的色度图显示，颜色分布是双峰的，达到我们的z〜1的红移极限，在0.2 1的星系部分。对于所有环境，该部分都朝着较低的红移和较高的发光度增加。与M_（g'）<-19.5的星系场相比，簇状区域内的红色分数随红移变化的速度加快了60％。我们首次使用跨分布在单个大体积中的许多簇场界面的观测结果，追踪了在近8 Gyr的时间内的大规模形态密度关系和Butcher-Oemler效应。

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