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Dark matter-only simulations predict that dark matter halos have steep, cuspyinner density profiles, while observations of dwarf galaxies find a range ofinner slopes that are often much shallower. There is debate whether thisdiscrepancy can be explained by baryonic feedback or if it may require modifieddark matter models. In Paper 1 of this series, we obtained high-resolutionintegral field H$\alpha$ observations for 26 dwarf galaxies with$M_*=10^{8.1}-10^{9.7}\textrm{M}_\odot$. We derived rotation curves from ourobservations, which we use here to construct mass models. We model the totalmass distribution as the sum of a generalized Navarro-Frenk-White (NFW) darkmatter halo and the stellar and gaseous components. Our analysis of the slopeof the dark matter density profile focuses on the inner 300-800 pc, chosenbased on the resolution of our data and the region resolved by modernhydrodynamical simulations. The inner slope measured using ionized andmolecular gas tracers is consistent, and it is additionally robust to thechoice of stellar mass-to-light ratio. We find a range of dark matter profiles,including both cored and cuspy slopes, with an average of $\rho_{\rm DM}\simr^{-0.74\pm 0.07}$, shallower than the NFW profile, but steeper than thosetypically observed for lower-mass galaxies with $M_*\sim10^{7.5}\textrm{M}_\odot$. Simulations that reproduce the observed slopes inthose lower-mass galaxies also produce slopes that are too shallow for galaxiesin our mass range. We therefore conclude that supernova feedback models do notyet provide a fully satisfactory explanation for the observed trend in darkmatter slopes.

The Dark Matter Distributions in Low-Mass Disk Galaxies. II. The Inner Density Profiles