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    Probing ISM Structure in Trumpler 14 and Carina I Using the Stratospheric Terahertz Observatory 2

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    Author
    Seo, Young Min
    Goldsmith, Paul F.
    Walker, Christopher K.
    Hollenbach, David J.
    Wolfire, Mark G.
    Kulesa, Craig A.
    Tolls, Volker
    Bernasconi, Pietro N.
    Kavak, Ümit
    van der Tak, Floris F. S.
    Shipman, Russ
    Gao, Jian Rong
    Tielens, Alexander
    Burton, Michael G.
    Yorke, Harold
    Young, Erick
    Peters, William L.
    Young, Abram
    Groppi, Christopher
    Davis, Kristina
    Pineda, Jorge L.
    Langer, William D.
    Kawamura, Jonathan H.
    Stark, Antony
    Melnick, Gary
    Rebolledo, David
    Wong, Graeme F.
    Horiuchi, Shinji
    Kuiper, Thomas B.
    Show allShow less
    Affiliation
    Univ Arizona, Dept Astron
    Univ Arizona, Steward Observ
    Issue Date
    2019-06-20
    Keywords
    ISM: kinematics and dynamics
    ISM: structure
    photon-dominated region (PDR)
    stars: formation
    surveys
    H II regions
    
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    Publisher
    IOP PUBLISHING LTD
    Citation
    Young Min Seo et al 2019 ApJ 878 120
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    Copyright © 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 observations of the Trumpler 14/Carina I region carried out using the Stratospheric Terahertz Observatory 2. The Trumpler 14/Carina I region is in the western part of the Carina Nebula Complex (CNC), which is one of the most extreme star-forming regions in the Milky Way. We observed Trumpler 14/Carina I in the 58 mu m transition of [C II] with a spatial resolution of 48 '' and a velocity resolution of 0.17 km s(-1). The observations cover a 0 degrees.25 by 0 degrees.28 area with central position l = 297 degrees.34, b = -0 degrees.60. The kinematics show that bright [C II] structures are spatially and spectrally correlated with the surfaces of CO clouds, tracing the photodissociation region (PDR) and ionization front of each molecular cloud. Along seven lines of sight (LOSs) that traverse Tr 14 into the dark ridge to the southwest, we find that the [C II] luminosity from the H II region is 3.7 times that from the PDR. In the same LOS, we find in the PDRs an average ratio of 1 : 4.1 : 5.6 for the mass in atomic gas : dark CO gas : molecular gas traced by CO. Comparing multiple gas tracers, including H I 21 cm, [C II], CO, and radio recombination lines, we find that the H II regions of the CNC are well described as H II regions with one side freely expanding toward us, consistent with the Champagne model of ionized gas evolution. The dispersal of the GMC in this region is dominated by EUV photoevaporation; the dispersal timescale is 20-30 Myr.
    ISSN
    0004-637X
    DOI
    10.3847/1538-4357/ab2043
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab2043
    Scopus Count
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    UA Faculty Publications

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