Poster Presentation

Kinematic Structure of Molecular Gas around Papillon Nebula in the Large Magellanic Cloud

Author(s): Kazuya Saigo (NAOJ), T. Onishi, K. Tokuda, R. Harada, Y. Morioka (Osaka Prefecture Univ.), O. Nayak, M. Meixner (Johns Hopkins), M. Sewilo (NASA), R. Indebetouw (NAO), A. Kawamura, T. Minamidani (NAOJ), K. Torii, K. Tachihara, Y. Fukui (Nagoya), et al.

Presenter: Kazuya Saigo (National Astronomical Observatory of Japan)

I report ALMA Band 3 and 6 results of 12CO(2-1), 13CO(2-1), H30a line, free-free emission around 98 GHz, and dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active high-mass star forming face-on galaxy at a distance 50kpc. It is the best target for studying high-mass star formation. Our ALMA observations show that N159E is the complex of filamentary clouds with the width of ~1pc and length of ~several pc. Total molecular mass is estimated to be 0.92 ×10^5 M_sun from the 13CO(2-1) intensity. N159E harbors the well-known Papillon Nebula, a compact HII region. We found that a YSO associated with the Papillon Nebula has the mass of 35M_sun and is located at the intersection of three filamentary clouds. Fukui et al. (2015a) reported a similar kinematic structure toward two YSOs of M ~ 35M_sun in the N159 West region. It suggests that the collision of filamentary clouds is a primary mechanism of high-mass star formation. We also report that physical conditions around Papillon Nebula. We found a sub-pc scale molecular hole around the YSO in Papillon Nebula. It is filled by free-free and H30a emission. Temperature of the molecular gas around the hole reaches 80 K. It indicates that this YSO has just started the destruction of parental molecular cloud.