Ratio of total mass M_total to stellar mass M within a spherical radius for the remnants of equal‐mass mergers of ﹩V_{\mathrm{vir}\,}=115﹩ km s⁻¹ disk galaxies with dark matter halos, star formation and supernova feedback as a function of progenitor gas content. The galaxy models are appropriate for ﹩z=0﹩ and are merged on nearly radial, parabolic orbits. Shown is M_total/M vs. R/R_e for remnants produced by progenitor systems with gas fraction ﹩f_{\mathrm{gas}\,}=0.01﹩ (red line), ﹩f_{\mathrm{gas}\,}=0.025﹩ (yellow line), ﹩f_{\mathrm{gas}\,}=0.04﹩ (green line), ﹩f_{\mathrm{gas}\,}=0.1﹩ (blue line), ﹩f_{\mathrm{gas}\,}=0.2﹩ (purple line), and ﹩f_{\mathrm{gas}\,}=0.4﹩ (black line). For small‐mass spheroidal remnants, as the progenitor gas content is increased the stellar content substantially increases in the very central regions (﹩R< 0.3R_{e}﹩) of the galaxy. The decrease in M_total/M follows the corresponding decrease in R_e as star formation is concentrated in the high central gas overdensities induced by the merger.