Spatially Resolved Interstellar Medium and Highly Excited Dense Molecular Gas in the Most Luminous Quasar at z = 6.327

Abstract

Among more than 200 quasars known at z 6, only one object, J0100+2802 (z=6.327), was found hosting a > 10 10 M super-massive black hole (SMBH). In order to investigate the host galaxy properties of J0100+2802, we performed multi-band ALMA observations, aiming at mapping the dust continuum, [C ii] and CO(6-5) emission lines with sub-kiloparsec scale resolution, as well as detecting high-J CO lines in CO(11-10), CO(10-9), and CO(7-6). The galaxy size is measured to be R major = 3.6 ± 0.2 kpc from the high resolution continuum observations. No ordered motion on kilo-parsec scales was found in both [C ii] and CO(6-5) emissions. The velocity dispersion is measured to be 161±7 km s −1 , ∼3 times smaller than that estimated from the local M-σ relation. In addition, we found that the CO emission is more concentrate (a factor of 1.8±0.4) than the [C ii] emission. Together with CO(2-1) detected by VLA, we measured the CO Spectral Line Energy Distribution (SLED), which is best fit by a two-components model, including a cool component at ∼ 24 K with a density of n (H 2 ) =10 4.5 cm −3 , and a warm component at ∼ 224 K with a density of n (H 2 ) =10 3.6 cm −3 . We also fitted the dust continuum with a graybody model, which indicates that it has either a high dust emissivity β 2 or a hot dust temperature T dust 60 K, or a combination of both factors. The highly excited CO emission and hot dust temperature suggest that the powerful AGN in J0100+2802 could contribute to the gas and dust heating although future observations are needed to confirm this.

The REQUIEM Survey. I. A Search for Extended Lyα Nebular Emission Around 31 z > 5.7 Quasars

“…Equation (1) implies that, for instance, a 10 2 M e remnant of a Population III star at z=30 needs to accrete at the Eddington limit for its entire life ( f Duty = 1) to reach a black hole mass >10 9 M e at z∼6, as observed in quasars (e.g., De Rosa et al 2011Mortlock et al 2011;Wu et al 2015;Mazzucchelli et al 2017;Bañados et al 2018;Pons et al 2019;Reed et al 2019;Shen et al 2019). In addition, investigations at mm and submm wavelengths also revealed that the host galaxies of these first quasars are vigorously growing in mass, with star formation rates   -M SFR 100 yr 1 (e.g., Walter et al 2009;Venemans et al 2012Venemans et al , 2016Venemans et al , 2018Wang et al 2013Wang et al , 2019aWillott et al 2015Willott et al , 2017Decarli et al 2018;Kim & Im 2019;Shao et al 2019;Yang et al 2019a).…”

“…mass of only ∼1.9×10 11 M e (Wang et al 2019a). Given this high luminosity, its proximity zone appears to be small [ = R p ( )  7.12 0.13 pMpc], implying that this quasar is relatively young, with a quasar age of t QSO ∼10 5 yr (Eilers et al 2017;Davies et al 2019b).…”

A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

“…For z∼2-4 submillimeter-selected galaxies (SMGs; Blain et al 2002), the measured dust-continuum emission appears 2-4 timesmore compact than the CO emission (Hodge et al 2015;Simpson et al 2015;Chen et al 2017;Calistro Rivera et al 2018). Similarly, for quasar host galaxies at z6 (studied with lower-resolution observations), the dust-continuum sizes also appear z∼2-4 times more compact than those of the CO (Feruglio et al 2018;Wang et al 2019). The dust-continuum and rest-frame optical (but not CO) sizes have also been compared in detail for SMGs (Hodge et al 2016(Hodge et al , 2019Gullberg et al 2019;Lang et al 2019); six massive and compact star-forming galaxies at z∼2.5 (Barro et al 2016); a z∼1.25 starburst (Nelson et al 2019); and massive, Hαselected galaxies at z∼2.2-2.5 (Tadaki et al 2017a).…”

SMBH seeds from dissipative dark matter

“…( 24), assuming that the locally observed scaling relations can be applied to high redshift galaxies. 6 compiled in [46,122] with the mass estimated using the virial method. The gray points are a more complete set of 196 quasars at z 6 compiled in [19], with the mass estimated indirectly from UV luminosity.…”

“…[123]. Observations [122,123,125] indicate that the host galaxies of massive, luminous quasars at z 6 have halo dynamical masses and velocity dispersions at least an order of magnitude lower than expected from the local M BH − M bulge and M BH − σ * v relations. However, as shown in Fig.…”