We compare the substructure evolution in pure dark matter ( DM ) halos with those in the presence of baryons , hereafter PDM and BDM models .
The prime halos have been analyzed in the previous work , Romano-Diaz et al .
Models have been evolved from identical initial conditions which have been constructed by means of the Constrained Realization method .
The BDM model includes star formation and feedback from stellar evolution onto the gas .
A comprehensive catalog of subhalo populations has been compiled and individual and statistical properties of subhalos analyzed , including their orbital differences .
We find that subhalo population mass functions in PDM and BDM are consistent with a single power law , M _ { sbh } ^ { \alpha } , for each of the models in the mass range of \sim 2 \times 10 ^ { 8 } ~ { } { M _ { \odot } } -2 \times 10 ^ { 11 } ~ { } { M _ { \odot } } .
However , we detect a nonnegligible shift between these functions , the time-averaged \alpha \sim - 0.86 for the PDM and -0.98 for the BDM models .
Overall , \alpha appears to be a nearly constant with variations of \pm 15 \% .
Second , we find that the radial mass distribution of subhalo populations can be approximated by a power law , R ^ { \gamma _ { sbh } } with a steepening that occurs at the radius of a maximal circular velocity , R _ { vmax } , in the prime halos .
Here we find that the \gamma _ { sbh } \sim - 1.5 for the PDM and –1 for the BDM models , when averaged over time inside R _ { vmax } .
The slope is steeper outside this region and approaches -3 .
We detect little spatial bias ( less than 10 \% ) between the subhalo populations and the DM distribution of the main halos .
Also , the subhalo population exhibits much less triaxiality in the presence of baryons , in tandem with the shape of the prime halo .
Finally , we find that , counter-intuitively , the BDM population is depleted at a faster rate than the PDM one within the central 30 kpc of the prime halo .
The reason for this is that although the baryons provide a substantial glue to the subhalos , the main halo exhibits the same trend .
This assures a more efficient tidal disruption of the BDM subhalo population .
However , this effect can be reversed for a more efficient feedback from stellar evolution and the central supermassive black holes , which will expel baryons from the center and decrease the central concentration of the prime halo .
We compare our results with via Lactea and Aquarius simulations and other published results .