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We compare the substructure evolution in pure dark matter (DM) halos withthose in the presence of baryons (PDM and BDM). The prime halos have beenanalyzed by Romano-Diaz et al (2009). Models have been evolved from identicalinitial conditions using Constrained Realizations, including star formation andfeedback. A comprehensive catalog of subhalos has been compiled and propertiesof subhalos analyzed in the mass range of 10^8 Mo - 10^11 Mo. We find thatsubhalo mass functions are consistent with a single power law, M_sbh^{alpha},but detect a nonnegligible shift between these functions, alpha -0.86 for thePDM, and -0.98 for the BDM. Overall, alpha const. in time with variations of+-15%. Second, we find that the radial mass distribution of subhalos can beapproximated by a power law, R^{gamma} with a steepening around the radius of amaximal circular velocity, Rvmax, in the prime halos. Gamma ~-1.5 for the PDMand -1 for the BDM, inside Rvmax, and is steeper outside. We detect littlespatial bias between the subhalo populations and the DM of the main halos. Thesubhalo population exhibits much less triaxiality with baryons, in tandem withthe prime halo. Finally, we find that, counter-intuitively, the BDM populationis depleted at a faster rate than the PDM one within the central 30kpc of theprime. Although the baryons provide a substantial glue to the subhalos, themain halos exhibit the same trend. This assures a more efficient tidaldisruption of the BDM subhalos. This effect can be reversed for a moreefficient feedback from stellar evolution and supermassive black holes, whichwill expel baryons from the center and decrease the concentration of the primehalo. We compare our results with via Lactea and Aquarius simulations and otherpublished results.

Dissecting Galaxy Formation: II. Comparing Substructure in Pure Dark Matter and Baryonic Models