Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud: II. 30 Doradus
With an aim of probing the physical conditions and excitation mechanisms of warm molecular gas in individual star-forming regions, we performed Herschel SPIRE Fourier Transform Spectrometer (FTS) observations of 30 Doradus in the Large Magellanic Cloud. In our FTS observations, important far-infrare...
Gespeichert in:
| Hauptverfasser: | , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
15 August 2019
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| In: |
Astronomy and astrophysics
Year: 2019, Jahrgang: 628 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/201935215 |
| Online-Zugang: | Verlag, Volltext: https://doi.org/10.1051/0004-6361/201935215 Verlag: https://www.aanda.org/10.1051/0004-6361/201935215 
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| Verfasserangaben: | M.-Y. Lee, S. C. Madden, F. Le Petit, A. Gusdorf, P. Lesaffre, R. Wu, V. Lebouteiller, F. Galliano, and M. Chevance |
MARC
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| 245 | 1 | 0 | |a Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud |b II. 30 Doradus |c M.-Y. Lee, S. C. Madden, F. Le Petit, A. Gusdorf, P. Lesaffre, R. Wu, V. Lebouteiller, F. Galliano, and M. Chevance |
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| 520 | |a With an aim of probing the physical conditions and excitation mechanisms of warm molecular gas in individual star-forming regions, we performed Herschel SPIRE Fourier Transform Spectrometer (FTS) observations of 30 Doradus in the Large Magellanic Cloud. In our FTS observations, important far-infrared (FIR) cooling lines in the interstellar medium, including CO J = 4-3 to J = 13-12, [C I] 370 µm, and [N II] 205 µm, were clearly detected. In combination with ground-based CO J = 1-0 and J = 3-2 data, we then constructed CO spectral line energy distributions (SLEDs) on ∼10 pc scales over a ∼60 pc × 60 pc area and found that the shape of the observed CO SLEDs considerably changes across 30 Doradus. For example, the peak transition Jp varies from J = 6-5 to J = 10-9, while the slope characterized by the high-to-intermediate J ratio α ranges from ∼0.4 to ∼1.8. To examine the source(s) of these variations in CO transitions, we analyzed the CO observations, along with [C II] 158 µm, [C I] 370 µm, [O I] 145 µm, H2 0-0 S(3), and FIR luminosity data, using state-of-the-art models of photodissociation regions and shocks. Our detailed modeling showed that the observed CO emission likely originates from highly compressed (thermal pressure P/kB ∼ 107-109 K cm−3) clumps on ∼0.7-2 pc scales, which could be produced by either ultraviolet (UV) photons (UV radiation field GUV ∼ 103-105 Mathis fields) or low-velocity C-type shocks (pre-shock medium density npre ∼ 104-106 cm−3 and shock velocity s ∼ 5-10 km s−1). Considering the stellar content in 30 Doradus, however, we tentatively excluded the stellar origin of CO excitation and concluded that low-velocity shocks driven by kiloparsec-scale processes (e.g., interaction between the Milky Way and the Magellanic Clouds) are likely the dominant source of heating for CO. The shocked CO-bright medium was then found to be warm (temperature T ∼ 100-500 K) and surrounded by a UV-regulated low-pressure component (P/kB ∼ a few (104-105) K cm−3) that is bright in [C II] 158 µm, [C I] 370 µm, [O I] 145 µm, and FIR dust continuum emission. | ||
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