Volume 525, January 2011
|Number of page(s)||9|
|Section||Interstellar and circumstellar matter|
|Published online||08 December 2010|
The HII region G35.673-00.847: another case of triggered star formation?
Instituto de Astronomía y Física del Espacio (IAFE),
CC 67, Suc. 28, 1428
2 FADU – Universidad de Buenos Aires, Argentina
Accepted: 18 October 2010
Aims. As part of a systematic study that we are performing to increase the observational evidence of triggered star formation in the surroundings of HII regions, we analyze the ISM around the HII region G35.673-00.847, a poorly studied source.
Methods. Using data from the large-scale surveys Two Micron All Sky Survey, Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), MIPSGAL, Galactic Ring Survey (GRS), VLA Galactic Plane Survey (VGPS), and NRAO VLA Sky Survey (NVSS), we performed a multiwavelength study of G35.673-00.847 and its surroundings.
Results. The mid-IR emission shows that G35.673-00.847 has an almost semi-ring like shape with a cut towards the galactic west. The radius of this semi-ring is about (~1.6 pc, at the distance of ~3.7 kpc). The distance was estimated from an HI absorption study and the analysis of the molecular gas. We find a molecular shell composed of several clumps distributed around the HII region, suggesting that its expansion is collecting the surrounding material. We identify several YSO candidates across the molecular shell. Finally, comparing the HII region dynamical age and the fragmentation time of the molecular shell, we discard the so-called collect and collapse as being the mechanism responsible for the YSO formation, suggesting that other processes such as radiative-driven implosion and/or small-scale Jeans gravitational instabilities operate.
Key words: HII regions / ISM: clouds / stars: formation
© ESO, 2010
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