论文标题
宇宙学21厘米线观测值，以测试超级 - 埃德丁顿积聚的黑洞是高红色超级大质量黑洞的种子
Cosmological 21cm line observations to test scenarios of super-Eddington accretion on to black holes being seeds of high-redshifted supermassive black holes
论文作者
论文摘要
在本文中，我们将超级 - 伊德丁顿积聚的场景研究到高红移$ z> 10 $的黑洞上，预计将是种子演变为超级质量的黑洞，直到红移$ z \ sim 7 $。对于初始质量，$ m _ {\ rm bh，ini} \ Lessim 2 \ times 10^{3} m _ {\ odot} $的种子BH，我们绝对需要超级 - 埃德丁顿积聚，这可以适用于天体物理学和原始起源。这样的吸积盘不可避免地发出高能光子，从而从高红移中连续加热了半乳酸间介质的宇宙学等离子体。在这种情况下，宇宙气温温度的宇宙历史被修改，宇宙学21 cm线的吸收特征被抑制。通过将21cm线吸收的理论预测与$ z \ sim17 $的观察数据进行比较，我们获得了质量上的宇宙学上限，这是种子BH质量的函数。为了实现$ m _ {\ rm bh} \ sim 10^9 m _ {\ odot} $ at $ z \ sim 7 $，通过连续的质量质量到种子BH，与宇宙学21厘米线的吸收在$ z \ sim z \ sim 17 $上是一致的，我们在$ z \ sim 17 $上获得了严重的上限，我们获得了$ $ $ $ $ bh，是$ $ bh，是$ bh，是$ bh，s s s s s s s s s s y hem n he s y he y he y he s y y y ym bh y m y y y y。 ini} \lesssim 10^2 M_{\odot}$ ($M_{\rm BH, ini} \lesssim 10^6 M_{\odot}$) when we assume a seed BH with its comoving number density $n_{\rm seed,0} \sim 10^{-3} {\rm mpc}^{ - 3} $（$ n _ {\ rm seed，0} \ sim 10^{ - 7} {\ rm mpc}^{ - 3} $）。我们还讨论了作为种子黑洞的原始黑洞的应用的一些含义。
In this paper, we study scenarios of the super-Eddington accretion onto black holes at high redshifts $z > 10$, which are expected to be seeds to evolve to supermassive black holes until redshift $z \sim 7$. For an initial mass, $M_{\rm BH, ini} \lesssim 2 \times 10^{3} M_{\odot}$ of a seed BH, we definitely need the super-Eddington accretion, which can be applicable to both astrophysical and primordial origins. Such an accretion disk inevitably emitted high-energy photons which had heated the cosmological plasma of the inter-galactic medium continuously from high redshifts. In this case, the cosmic history of cosmological gas temperature is modified, by which the absorption feature of the cosmological 21 cm lines is suppressed. By comparing theoretical predictions of the 21cm line absorption with the observational data at $z\sim17$, we obtain a cosmological upper bound on the mass-accretion rate as a function of the seed BH masses. In order to realize $M_{\rm BH} \sim 10^9 M_{\odot}$ at $z \sim 7$ by a continuous mass-accretion on to a seed BH, to be consistent with the cosmological 21cm line absorption at $z \sim 17$, we obtained an severe upper bound on the initial mass of the seed BH to be $M_{\rm BH, ini} \lesssim 10^2 M_{\odot}$ ($M_{\rm BH, ini} \lesssim 10^6 M_{\odot}$) when we assume a seed BH with its comoving number density $n_{\rm seed,0} \sim 10^{-3} {\rm Mpc}^{-3}$ ($n_{\rm seed,0} \sim 10^{-7} {\rm Mpc}^{-3}$). We also discuss some implications for application to primordial black holes as the seed black holes.
