Same as Figure 4, but for satellite dwarf galaxies in the isolated MW/M31 halos, which are matched in mass to the LG-like paired MW/M31 halos. For comparison, lighter dashed curves show averages from the paired halos from Figure 4. For low-mass satellites, those in the isolated halos are less likely to have been preprocessed in a group, at a level that is comparable to the halo-to-halo standard deviation. For high-mass satellites, any differences are well within the standard deviation.