Issue |
A&A
Volume 428, Number 3, December IV 2004
|
|
---|---|---|
Page(s) | 723 - 739 | |
Section | Astrophysical processes | |
DOI | https://doi.org/10.1051/0004-6361:20040485 | |
Published online | 07 December 2004 |
High-mass star formation within the bright-rimmed cloud SFO 79
1
Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, CT2 7NR, UK e-mail: jsu@star.kent.ac.uk
2
Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK
Received:
21
March
2004
Accepted:
29
July
2004
We report Radio Recombination Line (RRL) and continuum observations toward the IRAS point source
16362-4845, embedded within the Bright-Rimmed Cloud (BRC) SFO 79, a small molecular cloud lying at the
edge of the HII region RCW 108. High resolution observations of the H92α hydrogen recombination
line and of the continuum emission (3.6 and 6 cm) confirm the presence of a resolved Ultra Compact (UC) HII region embedded within the molecular cloud. The integrated radio fluxes suggest the source of the
ionisation to be an O9 Zero Age Main Sequence (ZAMS) star. Millimetre observations of 12CO,
13CO and C18O (–0) molecular lines reveal the presence of a molecular condensation
offset ~30´´ to the north of the IRAS position on the boundary of the UC HII region. Analysis of
2MASS data has led to the identification of a small IR cluster of Young Stellar Objects (YSOs) that are
positionally coincident with the UC HII region, lying to the south east of the peak of the radio emission.
Moreover, the UC HII region appears to be extended in the direction of the IR cluster, which suggests that
the radio emission and the IR cluster are in some way related to each other. MSX 8.3 μm and 21.3 μm images have been used to trace the large scale structure of the BRC, revealing the presence of a
Photo Dominated Region (PDR) and three embedded thermal sources within the molecular cloud. The PDR has a
plane parallel morphology which correlates extremely well with the morphology of the ionised gas traced by
the optical emission. The three thermal sources (labelled A, B, C) all lie at a similar projected distance
from the interface between the HII region and the molecular gas of the cloud. Thermal sources A and C are
positionally coincident with the IRAS point sources 16362–4845 and 16362–4841 respectively, both of which
have IRAS colours consistent with the presence of UC HII regions. Given that UC HII regions are relatively
short lived (~105 yrs) it is reasonable to suggest that these two UC HII regions are of a similar
age. The alignment of the three thermal sources along a line parallel to the bright rim suggests that they
could have been triggered by the propagation of a plane parallel shock through the cloud.
Key words: stars: formation / ISM: individual object: RCW 108, SFO 79 / ISM: clouds / ISM: HII regions / ISM: reflection nebulae / infrared: ISM
© ESO, 2004
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.