Large-Scale CI (3P1-- 3P0) and CO (J=3--2) Observations of the W51 Complex Region with the Mt. Fuji Submillimeter-Wave Telescope

Details Large-Scale CI (3P1-- 3P0) and CO (J=3--2) Observations of the W51 Complex Region with the Mt. Fuji Submillimeter-Wave Telescope Large-Scale CI (3P1-- 3P0) and CO (J=3--2) Observations of the W51 Complex Region with the Mt. Fuji Submillimeter-Wave Telescope

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc...88a&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

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We report mapping observations of CO (J=3-2) at 345.796 GHz and CI (3P1-3P0) at 492.161 GHz toward the W51 complex region using Mt. Fuji submillimeter-wave telescope. The mapped region is a {80' x 80'} area covering W51A, W51B, and W51C (SNR). The distribution of the CI emission is similar to that of the CO emission. The intensity map integrated over velocity from VLSR = 45 km s-1 to 55 km s-1 shows two intensity maxima, which coincide with two compact HII regions in W51A (G49.5-0.4 and G49.4-0.3). The intensity map integated over velocity from VLSR = 65 km s-1 to 72 km s-1 shows a molecular cloud elongated along W51A and W51B, which contains three clumps (one in W51A, the others in W51B). One of these clumps is associated with the non-thermal emission and an OH (1720 MHz) maser, and the interaction of SNR with the molecular cloud. The CI/CO integrated intensity ratio is 0.3-0.4 in W51A and W51B (HII region), while > 0.6 in W51B (OH maser). This result might imply that the interaction of SNR with the molecular cloud enhances the CI abundance.

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