Influences of accreting primordial black holes on the global 21 cm signal in the dark ages

Abstract

Baryonic matter can be accreted on to primordial back holes (PBHs) formed in the early Universe. The radiation from accreting PBHs is capable of altering the evolution of the intergalactic medium (IGM), leaving marks on the global 21 cm signal in the dark ages. For accreting PBHs with mass M PBH = 10 3 (10 4 ) M ⊙ and mass fraction f PBH = 10 −1 (10 −3 ), the brightness temperature deviation ∆δT b reaches ∼ 18 (26) mK at redshift z ∼ 90 (ν ∼ 16 MHz), and the gradient of the brightness temperature dδT b /dν reaches ∼ 0.8 (0.5) mK MHz −1 at frequency ν ∼ 28 MHz (z ∼ 50). For larger PBHs with higher mass fraction, the brightness temperature deviation is larger in the redshift range z ∼ 30 − 300 (ν ∼ 5 − 46 MHz), and the gradient is lower at the frequency range ν ∼ 20 − 60 MHz (z ∼ 23 − 70). It is impossible to detect these low frequency radio signals from the Earth due to the influence of the Earth's ionosphere. However, after taking care of the essential factors properly, e.g. the foreground and interference, future radio telescope in lunar orbit or on the farside surface of the Moon has a chance of detecting the global 21 cm signals impacted by accreting PBHs and distinguishing them from the standard model.

Cosmological 21cm line observations to test scenarios of super-Eddington accretion on to black holes being seeds of high-redshifted supermassive black holes

“…We can refer to papers for the other aspects of researches about the PBHs constrained from 21cm line observations for cosmological accretions on to PBHs[109,[123][124][125][126][127][128][129][130] and evaporation of PBHs[58,59,120,[131][132][133][134][135][136].…”