Spatially Resolved Interstellar Medium and Highly Excited Dense Molecular Gas in the Most Luminous Quasar at z = 6.327
AffiliationUniv Arizona, Steward Observ
quasars: individual (J0100+2802)
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PublisherIOP PUBLISHING LTD
CitationFeige Wang et al 2019 ApJ 880 2
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AbstractAmong more than 200 quasars known at z greater than or similar to 6, only one object, J0100+2802 (z = 6.327), was found hosting a >10(10) M-circle dot supermassive black hole. 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 subkiloparsec 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 kiloparsec scales was found in either the [C II] or the CO(6-5) emission. The velocity dispersion is measured to be 161 +/- 7 km s(-1), which is about three times smaller than that estimated from the local M-sigma relation. In addition, we found that the CO emission is more concentrated (a factor of 1.8 +/- 0.4) than the [C II] emission. Together with CO(2-1) detected by the Very Large Array (VLA), we measured the CO spectral line energy distribution, which is best fit by a two-component model that includes a cool component at similar to 24 K with a density of n((H2)) = 10(4.5) cm(-3), and a warm component at similar to 224 K with a density of n((H2)) = 10(3.6) cm(-3). We also fit the dust continuum with a graybody model. This indicated that the continuum has either a high dust emissivity beta greater than or similar to 2 or a hot dust temperature T-dust greater than or similar to 60 K, or a combination of these two factors. The highly excited CO emission and hot dust temperature suggest that the powerful active galactic nucleus in J0100+2802 could contribute to the gas and dust heating, but future observations are needed to confirm this.
VersionFinal published version
SponsorsNational Key R&D Program of China [2016YFA0400703]; National Science Foundation of China [11473004, 11533001, 11721303]; US NSF [AST-1515115]; NASA ADAP [NNX17AF28G]; VLA [VLA/14B-151, VLA/15A-494]; JCMT/SCUBA-2 [M15BI055]