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23 April 2024 |
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Probing ISM Structure in Trumpler 14 & Carina I Using The Stratospheric Terahertz Observatory 2 | | Young Min Seo
; Paul F. Goldsmith
; Chris Walker
; David J. Hollenbach
; Mark G. Wolfire
; Craig Kulesa
; Volker Tolls
; Pietro N. Bernasconi
; Umit Kavak
; Floris F.S. van der Tak
; Russ Shipman
; Jian Rong Gao
; Alexander Tielens
; Michael G. Burton
; Harold Yorke
; Erick Young
; William L. Peters
; Abram Young
; Christopher Groppi
; Kristina Davis
; Jorge L. Pineda
; William D. Langer
; Jonathan H. Kawamura
; Antony Stark
; Gary Melnick
; David Rebolledo
; Graeme F. Wong
; Shinji Horiuchi
; Thomas B. Kuiper
; | | Date: |
22 Mar 2019 | | Abstract: | We present observations of the Trumpler 14/Carina I region carried out using
the Stratospheric Terahertz Observatory 2 (STO2). The Trumpler 14/Carina I
region is in the west part of the Carina Nebula Complex, which is one of the
most extreme star-forming regions in the Milky Way. We observed Trumpler
14/Carina I in the 158 um transition of [CII] with a spatial resolution of 48"
and a velocity resolution of 0.17 km/s. The observations cover a 0.25 deg by
0.28 deg area with central position l = 297.34 deg, b = -0.60 deg. The
kinematics show that bright [CII] structures are spatially and spectrally
correlated with the surfaces of CO clouds, tracing the photodissociation region
and ionization front of each molecular cloud. Along 7 lines of sight that
traverse Tr 14 into the dark ridge to the southwest, we find that the [CII]
luminosity from the HII region is 3.7 times that from the PDR. In same los we
find in the PDRs a ratio of 1:4.1: 5.6 for the mass in atomic gas:dark-CO gas,
and gas traced by CO. Comparing multiple gas tracers including HI 21cm, [CII],
CO, and radio recombination lines, we find that the HII regions of the Carina
Nebula Complex are well-described as HII regions with one-side freely expanding
towards 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. | | Source: | arXiv, 1903.9517 | | Services: | Forum | Review | PDF | Favorites | |
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