Similar to Fig. 7 except that only a single redshift range is plotted (0.5 <z< 2), a redshift range which comprises the bulk of our sample. SPIRE-detected galaxies are broken into high-L_TIR (red filled circles), moderate-L_TIR (green filled squares), and low-L_TIR (blue filled diamonds) subsamples. Again in both the CMD (left) and CSMD (right), galaxies which went undetected or were not detected at high enough significance in the SPIRE imaging are shown as small black points. Histograms are normalized in the same way as Fig. 7 and arrows again represent the movement in each phase space when an stellar continuum extinction of E_s(B − V) = 0.3 is applied. Only those galaxies with K_s< 24.0 and stellar masses larger than the completeness limit (log (ℳ_∗) > 10.2) are plotted. While the LIRG subsamples show a high level of similarity in their M_NUV − M_r colors and M_r absolute magnitudes (left), the ULIRG population appears both bluer and brighter optically. The range of stellar masses spanned by the ULIRGs at any given color is generally larger than that of the LIRG samples (right) suggesting that the ULIRG population is inhomogenous, comprised of nascent galaxies undergoing their initial starbursts and older galaxies undergoing intense rejuvinated starburst events.