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Published August 20, 2017 | Version Published + Submitted
Journal Article Open

Gas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations

Creators

  • 1. ROR icon Peking University
  • 2. ROR icon National Radio Astronomy Observatory
  • 3. ROR icon New Mexico Institute of Mining and Technology
  • 4. ROR icon University of Cambridge
  • 5. ROR icon Max Planck Institute for Astronomy
  • 6. ROR icon California Institute of Technology
  • 7. ROR icon University of Arizona
  • 8. ROR icon Cornell University
  • 9. ROR icon University of Bonn
  • 10. ROR icon Princeton University
  • 11. ROR icon Institut d'Astrophysique de Paris
  • 12. ROR icon Haverford College
  • 13. ROR icon Max Planck Institute for Radio Astronomy

Abstract

We present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum and [C II] 158 μm 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 ~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 km s−1 at a radius of 3.2 kpc with an inclination angle of 34°. We measure the dynamical mass within the 3.2 kpc region to be 13.4^(+7.8)_(-5.3) x 10^(10) M⊙. This yields a black-hole and host galaxy mass ratio of 0.020^(+0.013)_(-0.007), which is about 4^(+3)_(-2) 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.

Additional Information

© 2017 The American Astronomical Society. Received 2017 May 26; revised 2017 July 10; accepted 2017 July 11; published 2017 August 18. This work was supported by the National Key Program for Science and Technology Research and Development (grant 2016YFA0400703) and the China Scholarship Council. G.C.J. is grateful for support from NRAO through the Grote Reber Doctoral Fellowship Program. D.R. acknowledges support from the National Science Foundation under grant number AST-1614213. R.W. acknowledges supports from the National Science Foundation of China (NSFC) grant Nos. 11473004 and 11533001 and the National Key Program for Science and Technology Research and Development (grant 2016YFA0400703). D.N. acknowledges support provided by the National Science Foundation via AST-1724864. We also thank professor D.J. Mortlock for providing the Gemini NIRI spectrum of J1319+0950. This work makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00206.S and ADS/JAO.ALMA#2012.1.00240.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Facility: ALMA - Atacama Large Millimeter Array.

Attached Files

Published - Shao_2017_ApJ_845_138.pdf

Submitted - 1707.03078.pdf

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Additional details

Identifiers

Eprint ID
80641
Resolver ID
CaltechAUTHORS:20170821-125059093

Related works

Describes
https://arxiv.org/abs/1707.03078 (URL)

Funding

National Key Program for Science and Technology Research and Development
2016YFA0400703
China Scholarship Council
National Radio Astronomy Observatory
NSF
AST-1614213
National Science Foundation of China
11473004
National Science Foundation of China
11533001
NSF
AST-1724864

Dates

Created
2017-08-21
Created from EPrint's datestamp field
Updated
2021-11-15
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Physics Department