Molecular gas and star formation in Sh2-196 and Sh2-206

Details Molecular gas and star formation in Sh2-196 and Sh2-206 Molecular gas and star formation in Sh2-196 and Sh2-206

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.114c&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

Astronomy and Astrophysics

Astronomy

Scientific paper

We report on a study of the HII regions Sh2-196 and Sh2-206 based on 12CO(1-0) line data from FCRAO and complementary radio continuum and HI-21 cm line data extracted from the CGPS, and infrared archive images, with the aim of investigating the interplay between the HII regions and the surrounding gas. The CO data allowed us to identify molecular gas linked to the HII regions. This molecular material partially borders the HII regions. In the case of Sh2-206, the distribution of the neutral atomic and molecular material is compatible with a blister-type HII region. To investigate the stellar formation activity in the environs of the nebulae we s earched for canditates to young stellar objects in the IRAS, MSX, and 2MASS point source catalogues, and analyzed their correlation with the molecular gas and interstellar dust. This study allowed the detection of molecular clumps linked to areas of active stellar formation in the center and the environs of Sh2-206, and in the environs of Sh2-196. The presence of young stellar objects in over- dense swept-up gas regions suggests that propagating star formation can not be discarded.

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