Artículo de revista
The 30 doradus molecular cloud at 0.4 pc resolution with the Atacama large millimeter/submillimeter array: physical properties and the boundedness of COemitting structures
Fecha
2022Registro en:
The Astrophysical Journal, 932:47 (19pp), 2022 June 10
10.3847/1538-4357/ac723a
Autor
Wong, Tony
Oudshoorn, Luuk
Sofovich, Eliyahu
Green, Alex
Shah, Charmi
Indebetouw, Rémy
Meixner, Margaret
Hacar, Alvaro
Nayak, Omnarayani
Tokuda, Kazuki
Bolatto, Alberto D.
Chevance, Mélanie
De Marchi, Guido
Fukui, Yasuo
Hirschauer, Alec S.
Jameson, K. E.
Kalari, Venu
Lebouteiller, Vianney
Looney, Leslie W.
Madden, Suzanne C.
Onishi, Toshikazu
Román Duval, Julia
Rubio López, Mónica Solange
Tielens, A. G. G. M.
Institución
Resumen
We present results of a wide-field (approximately 60 x 90 pc) Atacama Large Millimeter/submillimeter Array mosaic of CO(2-1) and (CO)-C-13(2-1) emission from the molecular cloud associated with the 30 Doradus star-forming region in the Large Magellanic Cloud (LMC). Three main emission complexes, including two forming a bow-tie-shaped structure extending northeast and southwest from the central R136 cluster, are resolved into complex filamentary networks. Consistent with previous studies, we find that the central region of the cloud has higher line widths at a fixed size relative to the rest of the molecular cloud and to other LMC clouds, indicating an enhanced level of turbulent motions. However, there is no clear trend in gravitational boundedness (as measured by the virial parameter) with distance from R136. Structures observed in (CO)-C-13 are spatially coincident with filaments and are close to a state of virial equilibrium. In contrast, (CO)-C-12 structures vary greatly in virialization, with low CO surface brightness structures outside of the main filamentary network being predominantly unbound. The low surface brightness structures constitute similar to 10% of the measured CO luminosity; they may be shredded remnants of previously star-forming gas clumps, or alternatively the CO-emitting parts of more massive, CO-dark structures.