Shock Excited H_2 Flows in OMC-2 and OMC-3

Details Shock Excited H_2 Flows in OMC-2 and OMC-3 Shock Excited H_2 Flows in OMC-2 and OMC-3

1997-06-08

arxiv.org/abs/astro-ph/9706073v1

Astronomy and Astrophysics

Astrophysics

9 pages, 6 figures, AAS style file required

Scientific paper

10.1086/310799

We report the discovery of nearly a dozen collimated outflows from young stellar objects embedded in the molecular filament that extends north of the Orion Nebula towards the H II region NGC 1977. The large number of nearly co-eval outflows and embedded class-0 young stellar objects indicates that the OMC-2/3 region is one of the most active sites of on-going low to intermediate mass star formation known. These outflows were identified in the 2.12 microns v=1-0 S(1) H_2 line during a survey of a 6 arcmin X 16 arcmin region containing the OMC-2 and OMC-3 cloud cores and over a dozen recently discovered class-0 protostars. We also observe filamentary emission that is likely to trace possible fluorescent H_2 in photo-dissociation regions associated with M 43 and NGC 1977. Neither the suspected outflows nor the fluorescent emission are seen at the continuum wavelength of 2.14 microns which confirms their emission line nature. Several of the new H_2 flows are associated with recently discovered bipolar molecular outflows. However, the most prominent bipolar CO outflow from the region (the MMS 8 flow) has no clear H_2 counterpart. Several H_2 flows consist of chains of knots and compact bow shocks that likely trace highly collimated protostellar jets. Our discovery of more than 80 individual H_2 emitting shocks demonstrate that outflows from young stars are churning this molecular cloud.

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