标题： UH8K弱透镜场中的星系聚类演化 显示英文标题

标题： Galaxy Clustering Evolution in the UH8K Weak Lensing Fields

摘要： 我们给出了双点星系角相关函数随视星等、颜色和形态的测量值。 我们给出了新的星系数目计数到I=24.0和V=25.0的极限星等。 我们发现 $\omega(\theta)$ 可以很好地用斜率-0.8的幂律描述。 我们发现相关函数的振幅随着视星等变暗单调减小。 我们将此与基于深红外观测的红移分布预测进行了比较。 我们得出结论，简单依赖于红移且通过ε参数表征演化的模型不能充分描述观测结果。 我们发现强聚类依赖于V-I颜色，因为极端颜色的星系位于相似的红移处，这些样本的角相关函数受随机投影稀释的程度最小。 然后，我们首次尝试利用相同形态类型和绝对光度的星系群体研究聚类的红移演化。 我们研究了Lstar早期型星系在0.2<z<0.9的红移范围内， $\omega(\theta)$ 对红移的依赖性。 尽管不确定性较大，但我们发现这些星系聚类的演化与稳定聚类[ε=0]一致。 我们发现Lstar早期型星系比局部全域星系稍微更强烈地聚类（rnought = 5.25\pm 0.28 \hMpc 假设ε=0）。 这与局部宇宙中Lstar早期型星系的2dFGRS值非常吻合（摘要）。 显示英文摘要

摘要： We present measurements of the two-point galaxy angular correlation function as a function of apparent magnitude, color, and morphology. We present new galaxy number counts to limiting magnitudes of I=24.0 and V=25.0. We find $\omega(\theta)$ to be well described by a power-law of slope -0.8. We find the amplitude of the correlation function to decrease monotonically with increasingly faint apparent magnitude. We compare with predictions utilizing redshift distributions based on deep spectroscopic observations. We conclude that simple redshift-dependent models which characterize evolution by means of the epsilon parameter inadequately describe the observations. We find a strong clustering dependence on V-I color because galaxies of extreme color lie at similar redshifts and the angular correlation functions for these samples are minimally diluted by chance projections. We then present the first attempt to investigate the redshift evolution of clustering, utilizing a population of galaxies of the same morphological type and absolute luminosity. We study the dependence of $\omega(\theta)$ on redshift for Lstar early-type galaxies in the redshift range 0.2<z<0.9. Although uncertainties are large, we find the evolution in the clustering of these galaxies to be consistent with stable clustering [epsilon=0]. We find Lstar early-type galaxies to cluster slightly more strongly (rnought = 5.25\pm0.28 \hMpc assuming epsilon=0) than the local full field population. This is in good agreement with the 2dFGRS value for Lstar early-type galaxies in the local universe (abridged).