标题： 新星巡天中的星系聚类：1 < z < 2之间恒星质量与暗物质晕质量的关系 显示英文标题

标题： Galaxy clustering in the NEWFIRM Medium Band Survey: the relationship between stellar mass and dark matter halo mass at 1 < z < 2

摘要： 我们利用NEWFIRM中深场巡天（NMBS）的数据，分析了红移1 < z < 2范围内星系的聚类与其恒星质量的关系。NMBS产生的精确光谱红移和恒星质量使我们能够定义一系列质量受限样本，这些样本包括比0.7、1和3×10^10太阳质量更大的星系，分别以z = 1.1、1.5和1.9为中心的红移区间。 在每个红移区间内，我们展示了聚类强度与样本恒星质量限制之间存在强烈的依赖关系，更高质量的星系在所有尺度上表现出更高的聚类幅度。我们进一步使用星系聚类的晕模型，在LCDM宇宙学背景下解释了我们的聚类测量结果。结果显示，中心星系和卫星星系的典型晕质量随着恒星质量的增加而增加，而卫星星系的比例则随恒星质量的增加而减少，这与z < 1时观察到的情况在定性上相同。 在我们的窄红移范围内，我们几乎没有发现恒星质量与晕质量关系的红移依赖性证据。然而，当我们与z~0附近的类似测量结果进行比较时，我们清楚地看到了这种关系的变化。如果我们假设一个普遍的重子分数，那么恒星质量与晕质量的比率揭示了被转化为恒星的重子比例。 我们看到，中央星系的恒星形成效率峰值在更高红移时向更高的晕质量移动，从z~0的约7×10^11太阳质量移动到z~1.5的约3×10^12太阳质量，揭示了"晕质量缩小"的证据。最后，我们显示，在z > 1的高偏倚星系群体中，测量的空间密度和聚类与晕模型预测的结果可能存在差异。 这可能意味着在这些红移处晕模型的一个或多个组成部分存在问题，例如晕偏置关系或晕分布。 显示英文摘要

摘要： We present an analysis of the clustering of galaxies as a function of their stellar mass at 1 < z < 2 using data from the NEWFIRM Medium Band Survey (NMBS). The precise photometric redshifts and stellar masses that the NMBS produces allows us to define a series of mass limited samples of galaxies more massive than 0.7, 1 and 3x10^10 Msun in redshift intervals centered on z = 1.1, 1.5 and 1.9 respectively. In each redshift interval we show that there exists a strong dependence of clustering strength on the stellar mass limit of the sample, with more massive galaxies showing a higher clustering amplitude on all scales. We further interpret our clustering measurements in the LCDM cosmological context using the halo model of galaxy clustering. We show that the typical halo mass of central and satellite galaxies increases with stellar mass, whereas the satellite fraction decreases with stellar mass, qualitatively the same as is seen at z < 1. We see little evidence of any redshift dependence in the stellar mass-to-halo mass relationship over our narrow redshift range. However, when we compare with similar measurements at z~0, we see clear evidence for a change in this relation. If we assume a universal baryon fraction, the ratio of stellar mass to halo mass reveals the fraction of baryons that have been converted to stars. We see that the peak in this star formation efficiency for central galaxies shifts to higher halo masses at higher redshift, moving from ~7x10^11 Msun at z~0 to ~3x10^12 Msun at z~1.5, revealing evidence of `halo downsizing'. Finally we show that for highly biased galaxy populations at z > 1 there may be a discrepancy between the measured space density and clustering and that predicted by the halo model. This could imply that there is a problem with one or more ingredients of the halo model at these redshifts, for instance the halo bias relation or the halo profile.