Abstract
Abstract
We report results of observations of the GGD 12-15 region, where cluster formation is actively taking place, using various molecular emission lines. The C18O (J = 1−0) emission line reveals a massive clump in the region with a mass of ∼2800 M
⊙ distributed over ∼2 pc. The distribution of the C18O (J = 3−2) emission is similar to that of a star cluster forming therein, with an elliptical shape of ∼1 pc in size. A bipolar molecular outflow driven by IRS 9Mc, a constituent star of the cluster, is blowing in the direction perpendicular to the elongated C18O (J = 3−2) distribution, covering the entire clump. There is a massive core with a radius of 0.3 pc and a mass of 530 M
⊙ in the center of the clump. There are two velocity components around the core, which are prominent in a position–velocity (PV) diagram along the major axis of the clump. In addition, a PV diagram along the minor axis of the clump, which is parallel to the outflow, shows a velocity gradient opposite to that of the outflow. The velocity structure strongly indicates the infalling motion of the clump. Comparison of the observational data with a simple model of infalling oblate clumps indicates that the clump is undergoing gravitational contraction with rotation.
Funder
Kayamori Foundation of Informational Science Advancement
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
1 articles.
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