论文标题
密度波动，光环丰度和聚集的功率谱与原始黑洞聚集
Power spectrum of density fluctuations, halo abundances and clustering with primordial black holes
论文作者
论文摘要
我们研究了将深色（DM）封装在原始黑洞（PBH）中的影响对密度波动$ p（k）$的功率谱的影响；我们还研究了它对光环及其聚类的影响。我们允许自物质和辐射平等以来的泊松波动的生长，并研究单色和扩展的PBH质量分布。我们通过要求$ <10 \％$ $偏离$λ$冷的暗物质功率频谱$ k = 1 $ k = 1 $ hmpc $^{ - 1} $，提出了更新的单色黑洞质量约束。我们的结果表明，具有质量$> 10^4 $ h $^{ - 1} m_ \ odot $的PBH被排除在宇宙中的所有DM中。我们还将这种条件应用于扩展的压力机（PS）质量函数，并发现泊松功率甚至在应用进化之前都取决于尺度。我们发现特征性质量$ m^*\ leq10^2 $ h $^{ - 1} m_ \ odot $，{与先前约束时，只剩下两个特征性的pbh质量质量窗口，在$ m^*\ sim10^2美元$ \ sim10^{ - 8} $ h $^{ - 1} m_ \ odot $，其中所有DM都可以在PBH中。这些窗口中产生的DM光晕质量功能与由基本颗粒制成的冷暗物质产生的DM质量功能相似。但是，一旦参数产生了不切实际的$ p（k）$，则产生的光环质量函数及其偏见作为光晕质量的函数，与在真实宇宙中测得的行为强烈偏离。
We study the effect of dark matter (DM) being encapsulated in primordial black holes (PBHs) on the power spectrum of density fluctuations $P(k)$; we also look at its effect on the abundance of haloes and their clustering. We allow the growth of Poisson fluctuations since matter and radiation equality and study both monochromatic and extended PBH mass distributions. We present updated monochromatic black hole mass constraints by demanding $<10\%$ deviations from the $Λ$ cold dark matter power spectrum at a scale of $k=1$hMpc$^{-1}$. Our results show that PBHs with masses $>10^4$h$^{-1}M_\odot$ are excluded from conforming all of the DM in the Universe. We also apply this condition to our extended Press-Schechter (PS) mass functions, and find that the Poisson power is scale dependent even before applying evolution. We find that characteristic masses $M^*\leq10^2 $h$^{-1}M_\odot$ are allowed, {leaving only two characteristic PBH mass windows of PS mass functions when combining with previous constraints, at $M^*\sim10^2$h$^{-1}M_\odot$ and $\sim10^{-8}$h$^{-1}M_\odot$ where all of the DM can be in PBHs. The resulting DM halo mass functions within these windows are similar} to those resulting from cold dark matter made of fundamental particles. However, as soon as the parameters produce unrealistic $P(k)$, the resulting halo mass functions and their bias as a function of halo mass deviate strongly from the behaviour measured in the real Universe.
