The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy. (arXiv:1812.06095v1 [astro-ph.GA])

The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy. (arXiv:1812.06095v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Leung_T/0/1/0/all/0/1">T. K. Daisy Leung</a> (1, 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">Dominik A. Riechers</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Baker_A/0/1/0/all/0/1">Andrew J. Baker</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Clements_D/0/1/0/all/0/1">Dave L. Clements</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Cooray_A/0/1/0/all/0/1">Asantha Cooray</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Hayward_C/0/1/0/all/0/1">Christopher C. Hayward</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Ivison_R/0/1/0/all/0/1">R. J. Ivison</a> (6, 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Neri_R/0/1/0/all/0/1">Roberto Neri</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Omont_A/0/1/0/all/0/1">Alain Omont</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_Fournon_I/0/1/0/all/0/1">Ismael Perez-Fournon</a> (10, 11), <a href="http://arxiv.org/find/astro-ph/1/au:+Scott_D/0/1/0/all/0/1">Douglas Scott</a> (12), <a href="http://arxiv.org/find/astro-ph/1/au:+Wardlow_J/0/1/0/all/0/1">Julie L. Wardlow</a> (13, 14) ((1) Cornell, (2) Flatiron, (3) Rutgers, (4) Imperial College London, (5) UC Irvine, (6) ESO, (7) Edinburgh, (8) IRAM, (9) Institut d'Astrophysique de Paris, (10) Instituto de Astrofisica de Canarias, (11) Universidad de La Laguna, (12) University of British Columbia, (13) Durham, (14) Lancaster)

We present CO(J= 1-0; 3-2; 5-4; 10-9) and 1.2-kpc resolution [CII] 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 hyper-luminous infrared galaxy
(LIR=(4+/-1)x10^13 Lsun) with a total molecular gas mass of (2.1+/-0.7)x10^11
(alpha_CO/0.8) Msun. The CO(J=1-0) and [CII] emission are extended over ~9 kpc
in diameter, and the CO line FWHM exceeds 1100 km s^-1. The [CII] 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)x10^11 Msun. We find a star formation rate (SFR) of 2900^750_-595
Msun yr^-1. HXMM05 is thus among the most intensely star-forming galaxies known
at high redshift. Photo-dissociation region modeling suggests physical
conditions similar to nearby SFGs, showing extended star formation, which is
consistent with our finding that the gas and dust emission are co-spatial. Its
molecular gas excitation resembles the local major merger Arp 220. The broad CO
and [CII] 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.

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