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The Molecular Ridge in the LMC extends several kiloparsecs south from 30Doradus, and it contains ~30% of the molecular gas in the entire galaxy.However, the southern end of the Molecular Ridge is quiescent - it containsalmost no massive star formation, which is a dramatic decrease from the veryactive massive star-forming regions 30 Doradus, N159, and N160. We present newALMA and APEX observations of the Molecular Ridge at a resolution as high as~16'' (~3.9 pc) with molecular lines 12CO(1-0), 13CO(1-0), 12CO(2-1),13CO(2-1), and CS(2-1). We analyze these emission lines with our new multi-linenon-LTE fitting tool to produce maps of T_kin, n_H2, and N_CO across the regionbased on models from RADEX. Using simulated data for a range of parameter spacefor each of these variables, we evaluate how well our fitting method canrecover these physical parameters for the given set of molecular lines. We thencompare the results of this fitting with LTE and X_CO methods of obtaining massestimates and how line ratios correspond with physical conditions. We find thatthis fitting tool allows us to more directly probe the physical conditions ofthe gas and estimate values of T_kin, n_H2, and N_CO that are less subject tothe effects of optical depth and line-of-sight projection than previousmethods. The fitted n_H2 values show a strong correlation with the presence ofYSOs, and with the total and average mass of the associated YSOs. Typical starformation diagnostics, such as mean density, dense gas fraction, and virialparameter do not show a strong correlation with YSO properties.

Physical Conditions in the LMC's Quiescent Molecular Ridge: Fitting Non-LTE Models to CO Emission