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    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

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

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The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy. / Leung, T. K. Daisy; Riechers, Dominik A.; Baker, Andrew J. et al.
In: The Astrophysical Journal, Vol. 871, No. 1, 85, 24.01.2019.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Leung, TKD, Riechers, DA, Baker, AJ, Clements, DL, Cooray, A, Hayward, CC, Ivison, RJ, Neri, R, Omont, A, Pérez-Fournon, I, Scott, D & Wardlow, JL 2019, 'The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy', The Astrophysical Journal, vol. 871, no. 1, 85. https://doi.org/10.3847/1538-4357/aaf860

APA

Leung, T. K. D., Riechers, D. A., Baker, A. J., Clements, D. L., Cooray, A., Hayward, C. C., Ivison, R. J., Neri, R., Omont, A., Pérez-Fournon, I., Scott, D., & Wardlow, J. L. (2019). The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy. The Astrophysical Journal, 871(1), Article 85. https://doi.org/10.3847/1538-4357/aaf860

Vancouver

Leung TKD, Riechers DA, Baker AJ, Clements DL, Cooray A, Hayward CC et al. The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy. The Astrophysical Journal. 2019 Jan 24;871(1):85. doi: 10.3847/1538-4357/aaf860

Author

Leung, T. K. Daisy ; Riechers, Dominik A. ; Baker, Andrew J. et al. / The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy. In: The Astrophysical Journal. 2019 ; Vol. 871, No. 1.

Bibtex

@article{fd3093035a9341118c0cd4ca776c4ca2,
title = "The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy",
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.",
keywords = "galaxies: evolution, galaxies: high-redshift, galaxies: kinematics and dynamics, photon-dominated region: PDR, quasars: individual: HXMM05, submillimeter: ISM",
author = "Leung, {T. K. Daisy} and Riechers, {Dominik A.} and Baker, {Andrew J.} and Clements, {Dave L.} and Asantha Cooray and Hayward, {Christopher C.} and Ivison, {R. J.} and Roberto Neri and Alain Omont and Ismael P{\'e}rez-Fournon and Douglas Scott and Wardlow, {Julie L.}",
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",
year = "2019",
month = jan,
day = "24",
doi = "10.3847/1538-4357/aaf860",
language = "English",
volume = "871",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "1",

}

RIS

TY - JOUR

T1 - The ISM Properties and Gas Kinematics of a Redshift 3 Massive Dusty Star-forming Galaxy

AU - Leung, T. K. Daisy

AU - Riechers, Dominik A.

AU - Baker, Andrew J.

AU - Clements, Dave L.

AU - Cooray, Asantha

AU - Hayward, Christopher C.

AU - Ivison, R. J.

AU - Neri, Roberto

AU - Omont, Alain

AU - Pérez-Fournon, Ismael

AU - Scott, Douglas

AU - Wardlow, Julie L.

N1 - 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

PY - 2019/1/24

Y1 - 2019/1/24

N2 - 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.

AB - 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.

KW - galaxies: evolution

KW - galaxies: high-redshift

KW - galaxies: kinematics and dynamics

KW - photon-dominated region: PDR

KW - quasars: individual: HXMM05

KW - submillimeter: ISM

U2 - 10.3847/1538-4357/aaf860

DO - 10.3847/1538-4357/aaf860

M3 - Journal article

VL - 871

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 85

ER -