The cores of dark matter-dominated galaxies: Theory versus observations

We use the rotation curves of a sample of dark matter-dominated dwarf and l ow surface brightness (LSB) late-type galaxies to study their radial mass d istributions. We find that the shapes of the rotation curves are remarkably similar for all (both dwarf and LSB) galaxies in the sample, suggesting a selfsimilar density distribution of their dark matter (DM) halos. This shap e can be reproduced well by a density profile with a shallow central cusp [ rho(r) proportional to 1/r(gamma), gamma approximate to 0.2-0.4] correspond ing to a steeply rising velocity curve [upsilon(r) proportional to r(g), g approximate to 0.9-0.8]. We further show that the observed shapes of the ro tation curves are well matched by the average density profiles of dark matt er halos formed in very high resolution simulations of the standard cold da rk matter model (CDM), the low-density CDM model with cosmological constant (Lambda CDM), and the cold + hot dark matter model with two types of neutr ino (CHDM). This is surprising in light of several previous studies, which suggested that the structure of simulated dark matter halos is inconsistent with the dynamics of dwarf galaxies. We discuss possible explanations for this discrepancy and show that it is most likely caused by the systematic d ifferences at small radii between the analytic model proposed by Navarro, F renk, & White, with gamma(NFW) = 1, and the actual central density profiles of the dark matter halos. We also show that the mass distributions in the hierarchically formed halos are on average consistent with the shape of rot ation curves of dark matter-dominated galaxies. However, the scatter of the individual profiles around the average is substantial. Finally, we show th at the dark matter halos in our hierarchical simulations and the real galax ies in our sample exhibit a similar decrease in their characteristic densit ies with increasing characteristic radial scales and show increase in their maximum rotation velocities with increase in the radii at which their maxi mum velocities occur.