http://arxiv.org/abs/1812.05527
There is a hope that looking into the early Universe with next-generation telescopes, one will be able to observe the early accretion growth of supermassive black holes (BHs) when their masses were $\sim 10^4$-$10^6 M_\odot$. According to the standard theory, the bulk of the gravitational potential energy released during radiatively efficient accretion onto a BH in this mass range is expected to fall into the extreme UV-ultrasoft X-ray band. We demonstrate that such a ‘miniquasar’ at $z\sim 15$ should leave a specific, localized imprint on the 21 cm cosmological signal. Namely, its position on the sky will be surrounded by a region with a fairly sharp boundary of several arcmin radius, within which the 21 cm brightness temperature quickly grows inwards from the background value of $\sim -200$ mK to $\sim +30$ mK. The size of this region is only weakly sensitive to the BH mass, so that the flux density of the excess 21 cm signal is expected to take a nearly universal value of $\sim 0.2[(1+z)/16]^{-2}$~mJy and should be detectable by the Square Kilometer Array. We argue that an optimal strategy would be to search for such signals from high-$z$ miniquasar candidates that can be found and localized with a next-generation X-ray mission such as Lynx. A detection of the predicted 21 cm signal would provide a measurement of the growing BH’s redshift to within $\Delta z/(1+z)<0.01$.
S. Sazonov and I. Khabibullin
Fri, 14 Dec 18
12/58
Comments: 13 pages, 16 figures, submitted to MNRAS