Home > Research > Publications & Outputs > The ISM Properties and Gas Kinematics of a Reds...

Associated organisational unit

Electronic data

  • 1812_06095

    Rights statement: This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.3847/1538-4357/aaf860

    Accepted author manuscript, 7.82 MB, PDF document

    Available under license: CC BY-NC: Creative Commons Attribution-NonCommercial 4.0 International License

Links

Text available via DOI:

View graph of relations

The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy

Research output: Contribution to journalJournal article

Published
  • T. K. Daisy Leung
  • Dominik A. Riechers
  • Andrew J. Baker
  • Dave L. Clements
  • Asantha Cooray
  • Christopher C. Hayward
  • R. J. Ivison
  • Roberto Neri
  • Alain Omont
  • Ismael Pérez-Fournon
  • Douglas Scott
  • Julie L. Wardlow
Close
Article number85
<mark>Journal publication date</mark>24/01/2019
<mark>Journal</mark>The Astrophysical Journal
Issue number1
Volume871
Number of pages29
Publication statusPublished
Original languageEnglish

Abstract

We present CO (J = 1 → 0 3 → 2 5 → 4 10 → 9) and 1.2 kpc resolution [C II] line observations of the dusty star-forming galaxy (SFG) HXMM05—carried out with the Karl G. Jansky Very Large Array, the Combined Array for Research in Millimeter-wave Astronomy, the Plateau de Bure Interferometer, and the Atacama Large Millimeter/submillimeter Array, measuring an unambiguous redshift of z = 2.9850 ± 0.0009. We find that HXMM05 is a hyperluminous infrared galaxy ({L}IR} = (4 ± 1) × 1013 L ⊙) with a total molecular gas mass of (2.1 ± 0.7) × 1011({α }CO}/0.8) M ⊙. The CO (J = 1 → 0) and [C II] emission are extended over ∼9 kpc in diameter, and the CO line FWHM exceeds 1100 km s‑1. The [C II] emission shows a monotonic velocity gradient consistent with a disk, with a maximum rotation velocity of {v}{{c}} = 616 ± 100 km s‑1 and a dynamical mass of (7.7 ± 3.1) × 1011 M ⊙. We find a star formation rate of 2900{}-595+750 M ⊙ yr‑1. HXMM05 is thus among the most intensely SFGs known at high redshift. Photodissociation region modeling suggests physical conditions similar to nearby SFGs, showing extended star formation, which is consistent with our finding that the gas emission and dust emission are cospatial. Its molecular gas excitation resembles the local major merger Arp 220. The broad CO and [C II] lines and a pair of compact dust nuclei suggest the presence of a late-stage major merger at the center of the extended disk, again reminiscent of Arp 220. The observed gas kinematics and conditions, together with the presence of a companion and the pair of nuclei, suggest that HXMM05 is experiencing multiple mergers as a part of the evolution.

Bibliographic note

This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.3847/1538-4357/aaf860