17μm molecular hydrogen line emission from OMC-1.
The v=0-0 S(1) line of molecular hydrogen at 17.03μm has been measured in the source OMC-1 along a 90'' cut passing through the near-IR H_2_ emission Peaks 1 and 2 using the Kuiper Airborne Observatory. The line flux is typically 50% of the 2.12μm v=1-0 S(1) line, but its distribution is somewhat more extended and it is relatively brighter at Peak 2. We interpret this as shocked emission coming from two regions of roughly equal brightness and lying close to the plane of the sky, plus a more extended contribution from slower shocks (~5km/s) which do not contribute significantly to the near-IR vibrational-rotational lines. The 17μm line flux is an order of magnitude too strong to be explained by planar J- and C-shock models. However our data cannot distinguish between the merits of a cooling flow dominated by H_2_ line emission and the integrated emission from a C-type bow-shock. Both models predict column density ratios close to those observed from a variety of lines covering a range from 1000 to 25000K in upper state energy. We predict a flux for the ground state 28.2μm 0-0 S(0) line of ~ 2% that of the 1-0 S(1) line at Peak1, and suggest that a consistent set of observations of the lowest pure rotational lines of H_2_ would allow us to distinguish between these shock models.
Astronomy and Astrophysics
- Pub Date:
- November 1997
- ISM: MOLECULES;
- ISM: INDIVIDUAL OBJECTS (OMC-1 = OMC 1);
- SHOCK WAVES;
- MOLECULAR PROCESSES;
- TECHNIQUES: SPECTROSCOPIC;
- INFRARED: ISM: LINES AND BANDS