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dc.contributor.authorWang, Feige
dc.contributor.authorWang, Ran
dc.contributor.authorFan, Xiaohui
dc.contributor.authorWu, Xue-Bing
dc.contributor.authorYang, Jinyi
dc.contributor.authorNeri, Roberto
dc.contributor.authorYue, Minghao
dc.date.accessioned2019-08-15T19:02:36Z
dc.date.available2019-08-15T19:02:36Z
dc.date.issued2019-07-17
dc.identifier.citationFeige Wang et al 2019 ApJ 880 2en_US
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/ab2717
dc.identifier.urihttp://hdl.handle.net/10150/633845
dc.description.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.en_US
dc.description.sponsorshipNational 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]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2019. The American Astronomical Society. All rights reserved.en_US
dc.subjectcosmology: observationsen_US
dc.subjectearly universeen_US
dc.subjectgalaxies: activeen_US
dc.subjectgalaxies: high-redshiften_US
dc.subjectquasars: individual (J0100+2802)en_US
dc.titleSpatially Resolved Interstellar Medium and Highly Excited Dense Molecular Gas in the Most Luminous Quasar at z = 6.327en_US
dc.typeArticleen_US
dc.identifier.eissn1538-4357
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.volume880
dc.source.issue1
dc.source.beginpage2
refterms.dateFOA2019-08-15T19:02:37Z


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