论文标题
红移21厘米的HI的宇宙黎明的黑洞
Black holes at cosmic dawn in the redshifted 21cm signal of HI
论文作者
论文摘要
宇宙黎明（CD）的流行III恒星和黑洞（BHS）的间接见解可能被印在21cm HI中的吸收信号，当时宇宙小于200 Myr时，在HI的21厘米线上。为了解释边缘报道的21厘米HI吸收的其他大幅度，基于BH-JET源的额外同步宇宙无线电背景（CRB）提出的模型，这些模型促进了CD处的HI吸收信号。最近观察到的高Z数量中的无线电大质量BHS（SMBHS）至z = 7，这表明存在着一个不明强度的z> 15的BHS中的CRB。为了匹配边缘的开始，需要向CMB的CRB发出可比强度的CRB。在这里，我们提供近似计算，以分析这种类型的吸收信号，以边缘为例。假设在z = 6-7时在类星体中〜10^9太阳能中观察到的BH质量与无线电亮度比率，我们发现，迅速增长的中间质量（IMBH）的无线电发光bhs在其中成为SMBH的唯一一个可以解释Z emply emples的smbhs的类型，该间隔是em emply的类型的sigbhs in thi smbhs。 18-20。在那些红移时，边缘信号将暗示IMBH的全球质量密度必须在恒星上占主导地位，这是预期在那些高红移时预期的最大恒星质量密度（SMD）的70％以上。这表明这些IMBH是以前形成的，并且比大量恒星生长更快，而典型的流行III星的恒星质量BH残留物没有大量贡献。可以在长无线电波长中检测到来自这些IMBH的高度红移信号，其中具有超敏干仪，例如SKA，在JWST的红外线中，以及在X射线检查中，并具有未来的太空任务。
Indirect insights of Pop III stars and Black Holes (BHs) at Cosmic Dawn (CD) may be imprinted as an absorption signal in the 21cm line of HI against the CMB, when the Universe was less than 200 Myr old. To explain the additional large amplitude of the 21cm HI absorption reported by EDGES there have been proposed models based on an additional synchrotron Cosmic Radio Background (CRB) from BH-jet sources that boost the HI absorption signal at CD. The recent observations of radio loud supermassive BHs (SMBHs) in high-z quasars up to z=7 suggest the existence of a CRB from growing BHs at z > 15, of unknown intensity. To match the onset of the EDGES signal a CRB of comparable intensity to that of the CMB is required. Here we provide approximate calculations to analyze this type of absorption signals, taking that of EDGES as an example. Assuming a BH mass to radio luminosity ratio as observed in radio-loud SMBHs of ~10^9 solar masses in quasars at z = 6-7, we find that rapidly growing radio luminous BHs of Intermediate Mass (IMBHs) in their way to become SMBHs, are the only type of astrophysical radio sources of a CRB that could explain the amplitude of the HI absorption reported by EDGES in the interval of z = 18-20. At those redshifts the EDGES signal would imply that the global mass density of IMBHs must be dominant over that of stars, more than 70% of the maximum Stellar Mass Density (SMD) expected at those high redshifts. This suggests that those IMBHs are formed before and grow faster than the bulk of stars, with no large mass contribution from stellar-mass BH remnants of typical Pop III stars. The highly redshifted signals from these IMBHs may be detected at long radio wavelengths with ultrasensitive interferometers such as the SKA, in the infrared with the JWST, and in the X-rays with future space missions.
