Probing ISM Structure in Trumpler 14 and Carina I Using the Stratospheric Terahertz Observatory 2
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Author
Seo, Young MinGoldsmith, 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.
Affiliation
Univ Arizona, Dept AstronUniv Arizona, Steward Observ
Issue Date
2019-06-20Keywords
ISM: kinematics and dynamicsISM: structure
photon-dominated region (PDR)
stars: formation
surveys
H II regions
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IOP PUBLISHING LTDCitation
Young Min Seo et al 2019 ApJ 878 120Journal
ASTROPHYSICAL JOURNALRights
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
0004-637XVersion
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/ab2043