Dark matter halos generated using standard initial conditions, as described in § 4.3. Halos of three different galactic‐type masses are shown; the intermediate‐mass halo (solid line) is the reference halo. Top left: log‐log density profiles. The lowest mass halo is not resolved at ≲1% of ﹩R_{\mathrm{vir}\,}﹩. An NFW ﹩c=10﹩ halo is shown for comparison (dot‐dashed line). Top right: Density profiles with the slope of ﹩\alpha =2﹩ divided out, so ﹩\alpha =2﹩ slopes are flat in this plot. Bottom right: Circular rotation curves. Bottom left: Distribution of SAMs in our halos, as histograms. For comparison, we include two extreme SAM distributions taken from N‐body simulations of van den Bosch et al. (2002).