自相互作用暗物质晕核心坍缩产生的高红移超大质量黑洞族群
High-redshift supermassive black hole population from core-collapse in self-interacting dark matter halos
- Indian Institute of Science Education and Research Berhampur（印度科学教育研究学院贝尔汉普尔分校）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究提出自相互作用暗物质晕核心坍缩可产生高红移超大质量黑洞种子，通过半解析模型预测并与观测对比，给出速度依赖的暗物质参数空间。
AI中文摘要：
暗物质（DM）粒子之间的自相互作用促进了DM晕中心区域内粒子间的能量再分配。近期关于大质量黑洞周围暗物质尖峰的研究，以及富含暗物质的低质量星系旋转曲线多样性，激发了人们对自相互作用截面$\mathcal{O}(10)\rm cm^2/gm$的探索。在如此高的散射率下，DM可以在某些宇宙学条件下，通过晕核心的引力热坍缩，导致超大质量黑洞种子的形成。宇宙黎明时期的类星体是检验高红移超大质量黑洞形成场景及其与结构形成联系的有力探针。在这项工作中，我们指出了有利的初始宇宙学条件，这些条件可能提供导致超大质量黑洞的黑洞种子，并通过自相互作用暗物质晕中的核心坍缩来介导。利用半解析的核心形成描述，以及现实的质量吸积和晕合并历史，我们将现有高红移超大质量黑洞的观测结果与我们的核心坍缩框架所预测的结果进行比较。我们发现，在爱丁顿吸积率为1的假设下，速度依赖的自相互作用暗物质参数空间的中值为$\sigma/m_{\chi}\sim 56\\,\rm cm^2/gm$和$\omega=101\\\\,\rm km/s$。对于亚爱丁顿和超爱丁顿吸积率，也给出了次主导值。我们还报告了推导出的自相互作用暗物质模型参数，以解释在高红移处观测到的分箱超大质量黑洞质量函数。
英文摘要：
Self-interactions between dark matter (DM) particles facilitate the inter-particle redistribution of energy within the central region of DM halos. Recent studies of dark matter spikes around massive black holes, and the diversity in rotation curves of dark matter rich low-mass galaxies motivate the exploration of self-interaction cross-section $\mathcal{O}(10)\,\rm cm^2/gm$. At such high scattering rates, DM can lead to the formation of supermassive black hole seeds, through the gravothermal collapse of halo cores, under certain cosmological conditions. Quasars near cosmic dawn are powerful probes for examining the formation scenario of high redshift supermassive black holes, and their connection to structure formation. In this work we point out the favorable initial cosmological conditions that are likely to provide the black hole seeds resulting in supermassive black holes, mediated by core-collapse in self-interacting dark matter halos. Employing a semi-analytic prescription of core formation, and realistic mass accretion and halo merger histories, we compare the existing observations of high-redshift supermassive black holes with those predicted for our core-collapse framework. We find the median values of velocity-dependent self-interacting dark matter parameter space $σ/m_χ\sim 56\, \rm cm^2/gm$, and $ω=101\,\rm km/s$, assuming an Eddington accretion rate of unity. Sub-leading values are also presented for sub and super-Eddington accretion rates. We also report the derived self-interacting dark matter model parameters to account for the observed binned supermassive black hole mass functions at high-redshifts.
