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    Source Structure and Molecular Gas Properties from High-resolution CO Imaging of SPT-selected Dusty Star-forming Galaxies

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    Dong_2019_ApJ_873_50.pdf
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    Author
    Dong, Chenxing
    Spilker, Justin S. cc
    Gonzalez, Anthony H.
    Apostolovski, Yordanka
    Aravena, Manuel cc
    Béthermin, Matthieu
    Chapman, Scott C.
    Chen, Chian-Chou cc
    Hayward, Christopher C.
    Hezaveh, Yashar D.
    Litke, Katrina C. cc
    Ma, Jingzhe
    Marrone, Daniel P.
    Morningstar, Warren R.
    Phadke, Kedar A.
    Reuter, Cassie A.
    Sreevani, Jarugula
    Stark, Antony A.
    Vieira, Joaquin D.
    Weiß, Axel
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2019-03-01
    Keywords
    galaxies: high-redshift
    galaxies: ISM
    gravitational lensing: strong
    ISM: molecules
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Chenxing Dong et al 2019 ApJ 873 50
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2019. The American Astronomical Society. All rights reserved.
    Collection Information
    This 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.
    Abstract
    We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of high-J CO lines (J(up) = 6, 7, 8) and associated dust continuum toward five strongly lensed, dusty, star-forming galaxies at redshift z = 2.7-5.7. These galaxies, discovered in the South Pole Telescope survey, are observed at 0.'' 2-0.'' 4 resolution with ALMA. Our high-resolution imaging coupled with the lensing magnification provides a measurement of the structure and kinematics of molecular gas in the background galaxies with spatial resolutions down to kiloparsec scales. We derive visibility-based lens models for each galaxy, accurately reproducing observations of four of the galaxies. Of these four targets, three show clear velocity gradients, of which two are likely rotating disks. We find that the reconstructed region of CO emission is less concentrated than the region emitting dust continuum even for the moderate-excitation CO lines, similar to what has been seen in the literature for lower-excitation transitions. We find that the lensing magnification of a given source can vary by 20%-50% across the line profile, between the continuum and line, and between different CO transitions. We apply Large Velocity Gradient modeling using apparent and intrinsic line ratios between lower-J and high-J CO lines. Ignoring these magnification variations can bias the estimate of physical properties of interstellar medium of the galaxies. The magnitude of the bias varies from galaxy to galaxy and is not necessarily predictable without high-resolution observations.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/ab02fe
    Version
    Final published version
    Sponsors
    University of Florida; McDonald Observatory at the University of Texas at Austin; Australian Government; Simons Foundation
    Additional Links
    http://stacks.iop.org/0004-637X/873/i=1/a=50?key=crossref.c0a55d4af888b6c0daa527f6db7f5014
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab02fe
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