Evidence for heavy-seed origin of early supermassive black holes from a z ≈ 10 X-ray quasar

Warning

This publication doesn't include Faculty of Sports Studies. It includes Faculty of Science. Official publication website can be found on muni.cz.
Authors

BOGDÁN Ákos GOULDING Andy D. NATARAJAN Priyamvada KOVÁCS Orsolya Eszter TREMBLAY Grant R. CHADAYAMMURI Urmila VOLONTERI Marta KRAFT Ralph P. FORMAN William R. JONES Christine CHURAZOV Eugene ZHURAVLEVA Irina

Year of publication 2024
Type Article in Periodical
Magazine / Source Nature Astronomy
MU Faculty or unit

Faculty of Science

Citation
Web https://www.nature.com/articles/s41550-023-02111-9
Doi http://dx.doi.org/10.1038/s41550-023-02111-9
Keywords Compact astrophysical objects; Early universe; Galaxies and clusters; High-energy astrophysics
Description Observations of quasars reveal that many supermassive black holes (BHs) were in place less than 700?Myr after the Big Bang. However, the origin of the first BHs remains a mystery. Seeds of the first BHs are postulated to be either light (that is, 10-100?M?), remnants of the first stars, or heavy (that is, 10-105?M?), originating from the direct collapse of gas clouds. Here, harnessing recent data from the Chandra X-ray Observatory, we report the detection of an X-ray-luminous massive BH in a gravitationally lensed galaxy identified by the James Webb Space Telescope at redshift z???10.3 behind the cluster lens Abell 2744. This heavily obscured quasar with a bolometric luminosity of ~5?×?1045?erg?s-1 harbours an ~107-108?M? BH assuming accretion at the Eddington limit. This mass is comparable to the inferred stellar mass of its host galaxy, in contrast to what is found in the local Universe wherein the BH mass is ~0.1% of the host galaxy’s stellar mass. The combination of such a high BH mass and large BH-to-galaxy stellar mass ratio just ~500?Myr after the Big Bang was theoretically predicted and is consistent with a picture wherein BHs originated from heavy seeds.
Related projects:

You are running an old browser version. We recommend updating your browser to its latest version.

More info