Kavli Affiliate: Ran Wang
| First 5 Authors: Yuxuan Wu, Tao Wang, Daizhong Liu, Qinghua Tan, Luis C. Ho
| Summary:
A significant population of quasars have been found to exist within the first
Gyr of cosmic time. Most of them have high black hole (BH) masses ($M_{rm BH}
sim 10^{8-10} M_{odot}$) with an elevated BH-to-stellar mass ratio compared
to typical local galaxies, posing challenges to our understanding of the
formation of supermassive BHs and their coevolution with host galaxies. Here,
based on size measurements of [CII] 158$mu$m emission for a statistical sample
of $z sim 6$ quasars, we find that their host galaxies are systematically more
compact (with half-light radius $R_{rm e} sim 1.6$ kpc) than typical
star-forming galaxies at the same redshifts. Specifically, the sizes of the
most compact quasar hosts, which also tend to contain less cold gas than their
more extended counterparts, are comparable to that of massive quiescent
galaxies at $z sim 4-5$. These findings reveal an intimate connection between
the formation of massive BHs and compactness of their host galaxies in the
early universe. These compact quasar hosts are promising progenitors of the
first population of quiescent galaxies.
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