Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.246m&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
The Orion molecular complex is the prototypical star forming region because of its proximity and vigorous star formation activity. This giant molecular cloud is a star nursery, where young massive stars and their strong stellar winds shape the parental molecular cloud, producing the collapse of new gas condensations and therefore triggering the formation of new stars. Fingerprints of star formation processes can be found everywhere in the cloud: hot cores, HII regions, circumstellar disks, outflows, Herbig-Haro objects, photodissociation regions, etc. All them reveal the strong interaction between young protostars and its surroundings. Being the most abundant molecular species in the universe after H_2, carbon monoxide (CO) provide the best way to study the distribution and kinematics of molecular gas in the universe. For that reason, a number of large scale CO maps have been performed in Orion. However, they lack the high spatial and/or spectral resolutions needed in order to better resolve the cloud structure and study its kinematics in detail. Our new 12CO and 13CO J=2-1 large scale maps (1 × 0.8°) observed with the IRAM 30-m telescope, have both high angular (˜11'') and velocity (˜0.4 km s-1) resolutions allowing us to resolve multiple line components and spatial structures at scales of 0.02 pc at a distance of 414 pc. These maps show numerous gas condensations and a complex velocity structure. In addition to the well-known "fingers", the central Orion cores and outflows (BN/KL, orion-S), and the Bar, these maps exhibit many filaments, cometary globules and cavities (or tunnels). All these structures are the result of massive star formation feedback on the molecular gas through the interaction with HII regions and powerful stellar winds. In this talk, besides the overall description of the gas distribution and kinematics, we will discuss the most interesting features we have found to be related with the M42 HII region expansion and/or the massive stellar winds present in the region.
Berné Olivier
Cernicharo Jose
Marcelino Nuria
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