论文标题
宇宙学限制对标量引起的重力波的原始黑洞的影响
Implications for primordial black holes from cosmological constraints on scalar-induced gravitational wave
论文作者
论文摘要
早期宇宙中足够大的标量扰动可以产生过度密度的区域，使原始黑洞（PBH）崩溃。该过程伴随着标量引起的重力波（SIGW）的发射，其行为像额外的辐射分量，因此有助于自由度（$ n _ {\ rm {eff}}} $）。我们表明，可以使用$ n _ {\ rm {eff}} $的宇宙学约束来对从这种特殊情况产生的PBH构成严格的限制，以及相关的小规模曲率扰动（$ \ \ \ \ \ m nathcal {p} _ _ {\ Mathcal {\ Mathcal {\ Mathcal {\ Mathcal {r r}} $）$）。我们表明，宇宙微波背景（CMB），Baryon声学振荡（BAO）和大爆炸核合成（BBN）数据集的组合可以排除具有峰值质量$ M _ {\ bulter} \ in [5 \ \ \ \ times 10^times 10^{5}，5} {5 \ \ inm peake $ m _ {\ buleart} \ inmmassive PBHS。 M} _ {\ odot} $作为暗物质的主要组成部分，而详细的约束取决于PBHS质量分布的形状。 CMB-S4（例如CMB-S4）的未来CMB任务可以将此约束窗口扩展到更大的范围$ m _ {\ bullet} \在[8 \ times 10^{ - 5}，5 \ times 10^{10}] \，{\ rm m m} _ {\ rm m} _ {\ odot} $，覆盖子类群体。 PBH上的这些限制对应于$ \ Mathcal {p} _ {\ Mathcal {r}} $的$ k \ in [10，10，10^{22}] \ in [10，10^{22}] \ rm {\ rm {mpc^{ - 1}}} $，比这些概率cmmb的comply and proce contect和comptraper的限制。
Sufficiently large scalar perturbations in the early Universe can create over-dense regions that collapse into primordial black holes (PBH). This process is accompanied by the emission of scalar-induced gravitational waves (SIGW) that behave like an extra radiation component, thus contributing to the relativistic degrees of freedom ($N_{\rm{eff}}$). We show that the cosmological constraints on $N_{\rm{eff}}$ can be used to pose stringent limits on PBHs created from this particular scenario as well as the relevant small-scale curvature perturbation ($\mathcal{P}_{\mathcal{R}}(k)$). We show that the combination of cosmic microwave background (CMB), baryon acoustic oscillation (BAO) and Big-Bang nucleosynthesis (BBN) datasets can exclude supermassive PBHs with peak mass $M_{\bullet} \in [5 \times 10^{5}, 5 \times 10^{10}]\,{\rm M}_{\odot}$ as the major component of dark matter, while the detailed constraints depend on the shape of the PBHs mass distribution. The future CMB mission like CMB-S4 can broaden this constraint window to a much larger range $M_{\bullet} \in [8 \times 10^{-5}, 5 \times 10^{10}]\,{\rm M}_{\odot}$, covering sub-stellar masses. These limits on PBH correspond to a tightened constraint on $\mathcal{P}_{\mathcal{R}}$ on scales of $k \in [10, 10^{22}]\ {\rm{Mpc^{-1}}}$, much smaller than those probed by direct CMB and large-scale structure power spectra.
