The Lambda CDM paradigm is largely successful at predicting large scale structures, however, there are several tensions with observations that exist at smaller scales, including the cusp-core problem and the diversity of rotation curves problem in dwarf galaxies. SIDM with a sufficiently large cross-section of interaction has been shown to naturally produce constant DM cores at the centers of dwarf halos, but strong constraints on the cross-section of interaction at different mass scales motivates the study of a velocity-dependent cross-section of interaction. In this talk I will present an analysis of core-collapse timescales and the distribution of dark matter at the centers of dwarf SIDM halos simulated with a velocity-dependent cross-section, from the new Ms. Marvel-Dark simulation. I contextualize our findings using results from the well studied CDM paradigm with a combination of dark matter only (DMO) simulations and simulations run with baryonic feedback from the MARVEL-ous collection of simulations.
