我们今天在哪里可以找到第一颗星的遗迹？
Where can we really find the First Stars' Remnants today?
摘要：
最近的一些数值研究表明，在极高红移下形成的稀有结构的残余，如最早的恒星和明亮的红移z~6类星体，优先位于红移z=0的最大质量星系团的中心。在本文中，我们重新讨论这个问题，结合使用宇宙学模拟的结构形成和扩展的Press-Schechter形式主义，我们表明，典型的第三星族恒星的遗迹，而不是更有可能被发现在一个群体的环境中，即在暗物质晕的质量~ 2 × 10 ^{13} h^{-1}M_sun。类似地，最明亮的z~6类星体的后代预计会出现在中等大小的星团（质量只有几个10^{14} h^{-1}M_sun）中，而不是在典型的1 Gpc ^3宇宙体积中发现的质量最大的超星团（M>10^{15} h^{-1}M_sun）中，明亮的z~6类星体就生活在这样的宇宙体积中。过去声称最大质量的星系团优先拥有这些残留物的起源是植根于用于初始化其数值模拟的数值方法：只有一个小区域的宇宙学体积的兴趣是模拟足够的分辨率，以识别低质量的晕在早期，这个区域被选择为托管最大质量的晕在宇宙学体积在晚期。因此，通过构建得出了这样的结论：在整个宇宙体积中形成的最早的结构在晚期演化成最大质量的晕。我们证明，相反，在宇宙学区域形成的第一个结构演变成相对典型的对象在以后的时间。我们提出了替代的数值方法来模拟宇宙体积中最早的结构。
英文摘要：
A number of recent numerical investigations concluded that the remnants of rare structures formed at very high redshift, such as the very first stars and bright redshift z~6 QSOs, are preferentially located at the center of the most massive galaxy clusters at redshift z=0. In this paper we readdress this question using a combination of cosmological simulations of structure formation and extended Press-Schechter formalism and we show that the typical remnants of Population III stars are instead more likely to be found in a group environment, that is in dark matter halos of mass ~2x10^{13} h^{-1}M_sun. Similarly, the descendants of the brightest z~6 QSOs are expected to be in medium-sized clusters (mass of a few 10^{14} h^{-1}M_sun), rather than in the most massive superclusters (M>10^{15} h^{-1}M_sun) found within the typical 1 Gpc^3 cosmic volume where a bright z~6 QSO lives. The origin of past claims that the most massive clusters preferentially host these remnants is rooted in the numerical method used to initialize their numerical simulations: Only a small region of the cosmological volume of interest was simulated with sufficient resolution to identify low-mass halos at early times, and this region was chosen to host the most massive halo in the cosmological volume at late times. The conclusion that the earliest structures formed in the entire cosmological volume evolve into the most massive halo at late times was thus arrived at by construction. We demonstrate that, to the contrary, the first structures to form in a cosmological region evolve into relatively typical objects at later times. We propose alternative numerical methods for simulating the earliest structures in cosmological volumes.
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