The environment and host haloes of the brightest z ~ 6 Lyman-break galaxies
The environment and host haloes of the brightest z ~ 6 Lyman-break galaxies
复制标题
最亮的 z ~ 6 莱曼断裂星系的环境和主晕
DOI：
10.1093/mnras/sty856
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发表时间：
2018
影响因子：
4.8
通讯作者：
Hatfield P
中科院分区：
文献类型：
--
作者：
Hatfield P
通过研究明亮的高红移莱曼破裂星系（LBG）种群的大尺度结构，可以深入了解早期宇宙中星系形成物理学中环境的作用。我们测量了一个明亮的（-22.7 <MUV<-21.125）LBG样本的聚类，并使用晕占据分布（HOD）模型来测量它们的典型晕质量。我们发现，集群振幅和相应的HOD拟合表明，这些来源是高度偏置（B 8）的对象在高红移宇宙的dennial地区。再加上观测到的这些天体的数密度的快速演化，我们的结果表明，光度函数的高光度端的形状与早期宇宙中的反馈过程或尘埃遮蔽有关-而不是这样一种情况，即这些源主要是处于特别活跃的星星形成时期的更多MUV −19星系群的罕见实例。有一个轻微的紧张局势之间的数量密度和聚类测量，我们解释这是一个信号，在高红移或准线性效应的结合模型晕偏置关系的细化可能需要在未来的尝试建模的聚类和数量计数。最后，字段之间的数密度的差异（UltraVISTA具有1.8倍以上的UDS的表面密度）被证明是一致的，与宇宙的聚类测量所暗示的方差。
By studying the large-scale structure of the bright high-redshift Lyman-break galaxy (LBG) population it is possible to gain an insight into the role of environment in galaxy formation physics in the early Universe. We measure the clustering of a sample of bright (−22.7 <MUV< −21.125) LBGs atz∼ 6 and use a halo occupation distribution (HOD) model to measure their typical halo masses. We find that the clustering amplitude and corresponding HOD fits suggests that these sources are highly biased (b∼ 8) objects in the densest regions of the high-redshift Universe. Coupled with the observed rapid evolution of the number density of these objects, our results suggest that the shape of high-luminosity end of the luminosity function is related to feedback processes or dust obscuration in the early Universe – as opposed to a scenario where these sources are predominantly rare instances of the much more numerousMUV∼ −19 population of galaxies caught in a particularly vigorous period of star formation. There is a slight tension between the number densities and clustering measurements, which we interpret this as a signal that a refinement of the model halo bias relation at high redshifts or the incorporation of quasi-linear effects may be needed for future attempts at modelling the clustering and number counts. Finally, the difference in number density between the fields (UltraVISTA has a surface density ∼ 1.8 times greater than UDS) is shown to be consistent with the cosmic variance implied by the clustering measurements.