Chandra Observations of the RCW 108 Star Forming Region.

Details Chandra Observations of the RCW 108 Star Forming Region. Chandra Observations of the RCW 108 Star Forming Region.

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20510506w&link_type=abstract

American Astronomical Society Meeting 205, #105.06; Bulletin of the American Astronomical Society, Vol. 36, p.1518

Astronomy and Astrophysics

Astronomy

Scientific paper

We present our recent (October 2004) Chandra observations of the embedded star forming region RCW 108. RCW 108 contains a deeply embedded young cluster lying in a dark cloud to the west of the young open cluster NGC 6193 (excited by two early O stars). Our motivation for this obsrvation was to followup on our discovery of diffuse X-ray emission in the older less embedded RCW 38. If the diffuse emission seen in RCW 38 is the result of plasma being trapped within the star forming region by overlaying molecular material, then RCW 108 should contain even more trapped plasma.
At 8-20 μ m microns, the Midcourse Space Experiment Galactic Plane Survey data shows a ridge of warm dust passing through the eastern edge of the emission peak parallel to but west of an optical ridge. Our SEST mm continuum observations show a cold component to this dust ridge peaking strongly at the cluster. The far infrared luminosity suggests that there is more than one significant heating source, i.e., OB stars and/or intermediate mass protostars. The extended infrared nebulosity to the east of the main cluster is due to emission and not reflection, suggesting a break-out of radiation in this direction.
The goals of the observations are to: 1) Study triggered star formation. 2) Investigate the origin and nature of diffuse X-ray emission within regions of massive star formation. 3) Identify deeply embedded PMS stars via their X-ray emission and derive an IMF and XLF. 4) Investigate the X-ray properties of the embedded sources.
This work is supported by the Chandra X-ray Center NASA contact NAS8-39073 and by the Chandra guest observer program.

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