arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 1809.01754astro-ph.GA
收藏

通过小宿主星系识别直接坍缩黑洞种子

Identifying Direct Collapse Black Hole Seeds through their Small Host Galaxies

Eli Visbal, Zoltan Haiman

备注：
7 pages, 3 figures, accepted by ApJL
阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

摘要：

对高红移类星体的观测表明，质量大于${\sim}10^9~M_\odot$的超大质量黑洞（SMBH）是在大爆炸后的前10亿年内聚集起来的。目前还不清楚如此大质量的黑洞是如何如此早形成的。一种可能的解释是，这些SMBH是由质量为$M_{\rm BH}\approx10^5~M_\odot$的“重”直接坍缩黑洞（DCBH）播种的，但观测尚未证实或反驳这种情况。在这封信中，我们利用宇宙学N体模拟来证明，在它们的质量增长大约一个数量级之前，DCBH的黑洞质量与晕质量之比将远远高于人口III（Pop III）恒星的黑洞残余物的预期，这些恒星已经增长到相同的质量（${\sim}10^6~M_\odot$）。我们还表明，当$T_{\rm vir}\approx 10^4~{\rm K}$晕（DCBH形成的潜在地点）合并与更大的附近的晕（$M_{\rm h} > 10^{10}~M_\odot$），他们几乎总是轨道与几个千秒差距，这是足够的空间分辨率与未来的X射线和红外望远镜的较大的主机晕。因此，我们建议，未来的X射线任务，如Lynx结合红外观测将能够区分高红移DCBH较小的黑洞种子由于异常高的黑洞质量恒星质量比的最微弱的类星体，推断BH质量低于${\sim} 10^6 M_\odot$。

英文摘要：

Observations of high-redshift quasars indicate that super massive black holes (SMBHs) with masses greater than ${\sim}10^9~M_\odot$ were assembled within the first billion years after the Big Bang. It is unclear how such massive black holes formed so early. One possible explanation is that these SMBHs were seeded by `heavy' direct collapse black holes (DCBHs) with masses of $M_{\rm BH}\approx10^5~M_\odot$, but observations have not yet confirmed or refuted this scenario. In this Letter, we utilize a cosmological N-body simulation to demonstrate that before they grow roughly an order of magnitude in mass, DCBHs will have black hole mass to halo mass ratios much higher than expected for black hole remnants of Population III (Pop III) stars which have grown to the same mass (${\sim}10^6~M_\odot$). We also show that when $T_{\rm vir}\approx 10^4~{\rm K}$ halos (the potential sites of DCBH formation) merge with much larger nearby halos ($M_{\rm h} > 10^{10}~M_\odot$), they almost always orbit their larger host halos with a separation of a few kpc, which is sufficient to be spatially resolved with future X-ray and infrared telescopes. Thus, we propose that a future X-ray mission such as Lynx combined with infrared observations will be able to distinguish high-redshift DCBHs from smaller black hole seeds due to the unusually high black hole mass to stellar mass ratios of the faintest observed quasars, with inferred BH masses below ${\sim} 10^6 M_\odot$.

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。

↑