Effective radius vs. halo mass, for all DLAs with identified host halos in runs A1 (diamonds), B1 (triangles), and C2 (crosses) at ﹩z=3﹩, for the fiducial background in Fig. 2. This figure does not account for DLAs caused by intergalactic H I clouds for which no host halo in the same base grid cell was found. The dotted horizontal line shows the size of the base grid cell in the ﹩8\ h^{-1}\ \mathrm{Mpc}\,﹩ volume. The solid lines are our least‐squares fits with eq. (8) for all halos from runs A1, B1, and C2 (thick line) and all halos from runs A1, B1, and C1 (thin line). For comparison, we have also plotted the fits to DLA radii from Nagamine et al. (2004), for models O3 (no wind, 10 Mpc volume; dashed line), Q3 (strong wind, 10 Mpc volume, low resolution; dashed‐dotted line), and Q5 (strong wind, 10 Mpc volume, high resolution; dotted line).