解释的虚空现象
The Void Phenomenon Explained
摘要：
我们使用高分辨率的N体模拟，结合星系偏差的晕占据模型，调查星系分布中的空隙。我们的目标是解决Peebles（2001）的“空洞现象”，它提出了观测到的空洞中微弱星系的缺乏，作为对当前宇宙学的挑战。在我们的模型中，星系的光度只被确定为暗物质晕质量的函数。通过这个简单的假设，我们证明了即使对于比L* 暗7个星等的星系，直径约为15 Mpc/h的大空洞也是可以预期的。我们的模型的预测是在良好的协议与几个统计措施：（i）在欠密区域的星系的光度函数，（ii）矮星系的最近邻统计，（iii）微弱星系的空概率函数。在暗物质中的暗丝和空洞之间的过渡中，晕质量函数突然改变，导致星系的最大光度在~1 Mpc/h的范围内降低~5个星等。因此，在星系分布中，暗条和空洞之间的边界对于矮星和~L* 天体几乎一样尖锐。这些结果支持了这样一种观点，即星系形成主要是由宿主暗物质晕的质量驱动的，并且几乎与大尺度晕环境无关。此外，他们证明了LCDM，结合一个简单的偏见模型，自然地解释了空洞现象的存在。
英文摘要：
We use high-resolution N-body simulations, combined with a halo occupation model of galaxy bias, to investigate voids in the galaxy distribution. Our goal is to address the 'void phenomenon' of Peebles (2001), which presents the observed dearth of faint galaxies in voids as a challenge to the current cosmology. In our model, galaxy luminosity is determined only as a function of dark matter halo mass. With this simple assumption, we demonstrate that large, empty voids of ~15 Mpc/h in diameter are expected even for galaxies seven magnitudes fainter than L*. The predictions of our model are in excellent agreement with several statistical measures; (i) the luminosity function of galaxies in underdense regions, (ii) nearest neighbor statistics of dwarf galaxies, (iii) the void probability function of faint galaxies. In the transition between filaments and voids in the dark matter, the halo mass function changes abruptly, causing the maximum galaxy luminosity to decrease by ~5 magnitudes over a range of ~1 Mpc/h. Thus the boundary between filaments and voids in the galaxy distribution is nearly as sharp for dwarfs as for ~L* objects. These results support a picture in which galaxy formation is driven predominantly by the mass of the host dark matter halo, and is nearly independent of the larger-scale halo environment. Further, they demonstrate that LCDM, combined with a straightforward bias model, naturally explains the existence of the void phenomenon.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
