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We used FIR and submillimeter continuum data from Herschel and the AtacamaPathfinder EXperiment (APEX) to fit pixel-by-pixel modified Planck SEDs toprestellar and protostellar clumps in the Census of High- and Medium-massProtostars (CHaMP) ($280^{\circ}<\ell<300^{\circ}$, $-4^{\circ}<b<+2^{\circ}$).We present maps of dust temperature ($T_{\text{d}}$) and H$_2$ column density(\ncol) for molecular clumps in the Carina Nebula complex (Regions 9 through11), and surrounding RCW 64 (Region 26). We compare the column densities of COand H$_2$ to chart regional variations in their correspondence, and derive mapsof the CO abundance. We find the CO abundance varies by an order of magnitudeor more across each region, averaging a few$\times$10$^{-5}$ CO per H$_2$, andthat the CO abundance distribution across each clump is correlated in both formand magnitude with environmental conditions, especially $T_{\text{d}}$. Thisdemonstrates that no single CO abundance suffices to convert from$N_{\text{CO}}$ to \ncol, even within a single molecular cloud. We also findthat $L/M$ traces $T_{\text{d}}$ almost exclusively, and therefore is not anindependent star formation tracer, but minima in $T_{\text{d}}$ almostuniversally coincide with maxima in \ncol, implying that cooling and densityenhancement must be simultaneous steps in prestellar clump evolution. Finally,based on generalized histogram N-PDFs of clump-scale (1-5 pc) and cloud-scale($\gtrsim10$ pc) samples, we could only obtain dual log-normal and power-lawfits to $\sim10\%$ of the clumps. The physical parameters derived from thesefits approach theoretical expectations, but have largely unknown uncertainties,so we advise treating the results of N-PDF fitting with caution.

On the Diagnostic Power of FIR/Sub-mm SED Fitting in Massive Galactic Molecular Clumps