Title
Star formation in bright-rimmed clouds. I. Millimeter and submillimeter molecular line surveys
Publication Date
2002
Journal or Book Title
ASTROPHYSICAL JOURNAL
Abstract
We present the results of the first detailed millimeter and submillimeter molecular line survey of bright-rimmed clouds, observed at FCRAO in the CO (J = 1 → 0), C18O (J = 1 → 0), HCO+ (J = 1 → 0), H13CO+ (J = 1 → 0), and N2H+ (J = 1 → 0) transitions, and at the Heinrich Hertz Telescope in the CO (J = 2 → 1), HCO+ (J = 3 → 2), HCO+ (J = 4 → 3), H13CO+ (J = 3 → 2), and H13CO+ (J = 4 → 3) molecular line transitions. The source list is composed of a selection of bright-rimmed clouds from the catalog of such objects compiled by Sugitani et al. We also present observations of three Bok globules done for comparison with the bright-rimmed clouds. We find that the appearance of the millimeter CO and HCO+ emission is dominated by the morphology of the shock front in the bright-rimmed clouds. The HCO+ (J = 1 → 0) emission tends to trace the swept-up gas ridge and overdense regions, which may be triggered to collapse as a result of sequential star formation. Five of the seven bright-rimmed clouds we observe seem to have an outflow; however, only one shows the spectral line blue-asymmetric signature that is indicative of infall in the optically thick HCO+ emission. We also present evidence that in bright-rimmed clouds the nearby shock front may heat the core from outside-in, thereby washing out the normally observed line infall signatures seen in isolated star-forming regions. We find that the derived core masses of these bright-rimmed clouds are similar to other low- and intermediate-mass star-forming regions.
DOI
10.1086/342237
Pages
798-825
Volume
577
Issue
2
Recommended Citation
De Vries, CH; Narayanan, Gopal; and Snell, Ronald L., "Star formation in bright-rimmed clouds. I. Millimeter and submillimeter molecular line surveys" (2002). ASTROPHYSICAL JOURNAL. 623.
10.1086/342237
Comments
This is the pre-published version harvested from ArXiv. The published version is located at http://iopscience.iop.org/0004-637X/577/2/798/