Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.6504t&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #65.04; Bulletin of the American Astronomical Society, Vol. 24, p.1222
Other
Scientific paper
Three molecular cloud regions in M33 have been mapped in the (12) CO J=2-1 line. Incorporating previously taken J=1-0 data, (12) CO line ratios were calculated in these regions to determine whether the line ratios, and hence the physical conditions, vary from one region to another within the galaxy. By studying a nearby galaxy such as M33, we can measure spatial variation of this ratio on scales of 100-200 pc. Two regions are centered on molecular clouds in the inner disk, MC19 and MC32. The third is centered on the giant HII region NGC 595, in a region where the star formation rates and efficiencies are higher than those of the inner disk by an order of magnitude. Despite this range of conditions, there is no significant difference between the ratios found for gas in the direction of NGC 595 and those found for the inner disk regions. On average in all three regions, the ratio of J=2-1 to J=1-0 integrated intensities is about 0.70, with one position in the MC32 region where R is greater than 1. This result suggests that density has a stronger influence on the value of the ratio than temperature. This idea is supported by the fact that the position of high ratio value does not correspond with any HII regions as seen in Hα . In order to fit the line ratios to physical parameters, both LTE and LVG (large velocity gradient) approximations are used.
Thornley Michele D.
Wilson Christine Diana
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