Estimating the spins of supermassive black holes in distant ultraluminous quasars

TL;DR

This study estimates the spins, inclination angles, and masses of supermassive black holes in distant ultraluminous quasars, revealing high spins and strong parameter correlations that suggest rapid growth via disk accretion.

Contribution

It provides the first estimates of SMBH spins in quasars at redshifts 6 to 7.5, showing high spin values and their correlation with other parameters, indicating efficient accretion-driven growth.

Findings

Estimated SMBH spins are generally greater than 0.9.

Strong correlations exist between spin, inclination, and mass.

High accretion rates likely drive rapid SMBH growth in early quasars.

Abstract

We estimated spin, inclination angle and corresponding SMBH mass values for sample of extremely distant (6 < z < 7.5) ultraluminous quasars. The estimated spin values are on average greater that 0.9 and the spin distribution has a characteristic appearance, similar to ones obtained for other types of AGNs and quasars. The dependence of estimated parameters on each other shows strong correlations between them, from which we can assume that in this early quasars the growth of SMBHs mass should occur mainly due to disk accretion with high accretion rate, which very effectively increases the spin.