Astrophys. J., 886, 15-15 (2019/November-3)
An ALMA view of molecular filaments in the Large Magellanic Cloud. II. An early stage of high-mass star formation embedded at colliding clouds in N159W-South.
TOKUDA K., FUKUI Y., HARADA R., SAIGO K., TACHIHARA K., TSUGE K., INOUE T., TORII K., NISHIMURA A., ZAHORECZ S., NAYAK O., MEIXNER M., MINAMIDANI T., KAWAMURA A., MIZUNO N., INDEBETOUW R., SEWILO M., MADDEN S., GALAMETZ M., LEBOUTEILLER V., CHEN C.-H.R. and ONISHI T.
Abstract (from CDS):
We have conducted ALMA CO isotopes and 1.3 mm continuum observations toward filamentary molecular clouds of the N159W-South region in the Large Magellanic Cloud with an angular resolution of ∼0.''25 (∼0.07 pc). Although the previous lower-resolution (∼1'') ALMA observations revealed that there is a high-mass protostellar object at an intersection of two line-shaped filaments in 13CO with the length scale of ∼10 pc, the spatially resolved observations, in particular, toward the highest column density part traced by the 1.3 mm continuum emission, the N159W-South clump, show complicated hub-filamentary structures. We also discovered that there are multiple protostellar sources with bipolar outflows along the massive filament. The redshifted/blueshifted components of the 13CO emission around the massive filaments/protostars have complementary distributions, which is considered to be possible evidence for a cloud-cloud collision. We propose a new scenario in which the supersonically colliding gas flow triggers the formation of both the massive filament and protostars. This is a modification of the earlier scenario of cloud-cloud collision, by Fukui et al., that postulated the two filamentary clouds occur prior to the high-mass star formation. A recent theoretical study of the shock compression in colliding molecular flows by Inoue et al. demonstrates that the formation of filaments with hub structure is a usual outcome of the collision, lending support for the present scenario. The theory argues that the filaments are formed as dense parts in a shock compressed sheet-like layer, which resembles "an umbrella with pokes."
© 2019. The American Astronomical Society. All rights reserved.
ISM: clouds - ISM: individual objects: N159W - ISM: kinematics and dynamics - stars: formation - stars: protostars
Fig. 1, Tables 1-2: [TFH2019] N159W MMS-N (Nos MMS-1 to MMS-4), [TFH2019] N159W YSO-SN N=1.
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