Ratio of M_total to M with spherical radius for the remnants of equal‐mass mergers of ﹩V_{\mathrm{vir}\,}=500﹩ 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 large‐mass spheroidal remnants, as the progenitor gas content is increased the central stellar content begins to increase substantially after ﹩R\gtrsim 0.3R_{e}﹩. The M_total/M value near the center is larger for massive systems than for less‐massive spheroids (see Fig. 14), reflecting the increasing importance of dark matter at the center of massive spheroidal galaxies.