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We present a complete 12CO J = 1-0 map of the prominent molecular ridge inthe Large Magellanic Cloud (LMC) obtained with the 22-m ATNF Mopra Telescope.The region stretches southward by ~2 degrees, (or 1.7kpc) from 30 Doradus, themost vigorous star-forming region in the Local Group. The location of thismolecular ridge is unique insofar as it allows us to study the properties ofmolecular gas as a function of the ambient radiation field in a low-metallicityenvironment. We find that the physical properties of CO-emitting clumps withinthe molecular ridge do not vary with the strength of the far-ultraviolet (FUV)radiation field. Since the peak CO brightness of the clumps shows nocorrelation with the radiation field strength, the observed constant value forCO-to-H_2 conversion factor along the ridge seems to require an increase in thekinetic temperature of the molecular gas that is offset by a decrease in theangular filling factor of the CO emission. We find that the difference betweenthe CO-to-H_2 conversion factor in the molecular ridge and the outer Milky Wayis smaller than has been reported by previous studies of the CO emission:applying the same cloud identification and analysis methods to our COobservations of the LMC molecular ridge and CO data from the outer Galaxysurvey by Dame et al. (2001), we find that the average CO-to-H_2 conversionfactor in the molecular ridge is X_CO = (3.9+/-2.5)10^20 cm^-2 (K km s^-1)^-1,approximately twice the value that we determine for the outer Galaxy clouds.The mass spectrum and the scaling relations between the properties of the COclumps in the molecular ridge are similar, but not identical, to those thathave been established for Galactic molecular clouds.

The Influence of Far-Ultraviolet Radiation on the Properties of Molecular Clouds in the 30 Dor Region of the Large Magellanic Cloud