Probing ISM Structure in Trumpler 14 & Carina I Using The Stratospheric Terahertz Observatory 2
| Autor: | Seo, Young Min, Goldsmith, Paul F., Walker, Chris, Hollenbach, David J., Wolfire, Mark G., Kulesa, Craig, Tolls, Volker, Bernasconi, Pietro N., Kavak, Umit, 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. |
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| Rok vydání: | 2019 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| DOI: | 10.3847/1538-4357/ab2043 |
| Popis: | 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 $\mu$m transition of [C\,{\sc ii}] with a spatial resolution of 48$''$ and a velocity resolution of 0.17 km s$^{-1}$. The observations cover a 0.25$^\circ$ by 0.28$^\circ$ area with central position {\it l} = 297.34$^\circ$, {\it b} = -0.60$^\circ$. The kinematics show that bright [C\,{\sc ii}] 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 [C\,{\sc ii}] luminosity from the HII region is 3.7 times that from the PDR. In 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 HI 21cm, [C\,{\sc ii}], 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. Comment: ApJ accepted |
| Databáze: | arXiv |
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