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dc.contributor.authorShao, Yali
dc.contributor.authorWang, Ran
dc.contributor.authorJones, Gareth C.
dc.contributor.authorCarilli, Chris L.
dc.contributor.authorWalter, Fabian
dc.contributor.authorFan, Xiaohui
dc.contributor.authorRiechers, Dominik A.
dc.contributor.authorBertoldi, Frank
dc.contributor.authorWagg, Jeff
dc.contributor.authorStrauss, Michael A.
dc.contributor.authorOmont, Alain
dc.contributor.authorCox, Pierre
dc.contributor.authorJiang, Linhua
dc.contributor.authorNarayanan, Desika
dc.contributor.authorMenten, Karl M.
dc.date.accessioned2017-10-03T15:43:11Z
dc.date.available2017-10-03T15:43:11Z
dc.date.issued2017-08-18
dc.identifier.citationGas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations 2017, 845 (2):138 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aa826c
dc.identifier.urihttp://hdl.handle.net/10150/625774
dc.description.abstractWe present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum and [C II] 158 mu m fine structure line emission toward a far-infrared-luminous quasar, ULAS J131911.29+095051.4 at z = 6.13, and combine the new Cycle 1 data with ALMA Cycle 0 data. The combined data have an angular resolution of similar to 0.'' 3, and resolve both the dust continuum and the [C II] line emission on a few kiloparsec scales. The [C II] line emission is more irregular than that of the dust continuum emission, which suggests different distributions between the dust and the [C II] emitting gas. The combined data confirm the [C II] velocity gradient that we had previously detected in a lower-resolution ALMA image from the Cycle 0 data alone. We apply a tilted ring model to the [C II] velocity map to obtain a rotation curve, and constrain the circular velocity to be 427 +/- 55 kms(-1) at a radius of 3.2 kpc with an inclination angle of 34 degrees. We measure the dynamical mass within the 3.2 kpc region to be 13.4(-5.3)(+7.8) x 10(10) M-circle dot. This yields a black-hole and host galaxy mass ratio of 0.020(-0.007)(+0.013), which is about 4(-2)(+3) times higher than that of the present-day M-BH/M-bulge ratio. This suggests that the supermassive black hole grows the bulk of its mass before the formation of most of the stellar mass in this quasar host galaxy in the early universe.
dc.description.sponsorshipNational Key Program for Science and Technology Research and Development [2016YFA0400703]; China Scholarship Council; NRAO through the Grote Reber Doctoral Fellowship Program; National Science Foundation [AST-1614213, AST-1724864]; National Science Foundation of China (NSFC) [11473004, 11533001]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/845/i=2/a=138?key=crossref.2da899d679a2133feb0b92fb99f48214en
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectgalaxies: activeen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: high-redshiften
dc.subjectquasars: generalen
dc.subjectradio lines: galaxiesen
dc.subjectsubmillimeter: galaxiesen
dc.titleGas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observationsen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
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
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-18T10:28:42Z
html.description.abstractWe present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum and [C II] 158 mu m fine structure line emission toward a far-infrared-luminous quasar, ULAS J131911.29+095051.4 at z = 6.13, and combine the new Cycle 1 data with ALMA Cycle 0 data. The combined data have an angular resolution of similar to 0.'' 3, and resolve both the dust continuum and the [C II] line emission on a few kiloparsec scales. The [C II] line emission is more irregular than that of the dust continuum emission, which suggests different distributions between the dust and the [C II] emitting gas. The combined data confirm the [C II] velocity gradient that we had previously detected in a lower-resolution ALMA image from the Cycle 0 data alone. We apply a tilted ring model to the [C II] velocity map to obtain a rotation curve, and constrain the circular velocity to be 427 +/- 55 kms(-1) at a radius of 3.2 kpc with an inclination angle of 34 degrees. We measure the dynamical mass within the 3.2 kpc region to be 13.4(-5.3)(+7.8) x 10(10) M-circle dot. This yields a black-hole and host galaxy mass ratio of 0.020(-0.007)(+0.013), which is about 4(-2)(+3) times higher than that of the present-day M-BH/M-bulge ratio. This suggests that the supermassive black hole grows the bulk of its mass before the formation of most of the stellar mass in this quasar host galaxy in the early universe.


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