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We present a suite of FIRE-2 cosmological zoom-in simulations of isolatedfield dwarf galaxies, all with masses of $M_\mathrm{halo} \approx10^{10}\,$M$_\odot$ at $z=0$, across a range of dark matter models. For thefirst time, we compare how both self-interacting dark matter (SIDM) and/or warmdark matter (WDM) models affect the assembly histories as well as the centraldensity structure in fully hydrodynamical simulations of dwarfs. Dwarfs withsmaller stellar half-mass radii (r$_{1/2}<500$ pc) have lower$\sigma_\star/V_\mathrm{max}$ ratios, reinforcing the idea that smaller dwarfsmay reside in halos that are more massive than is naively expected. Themajority of dwarfs simulated with self-interactions actually experiencecontraction of their inner density profiles with the addition of baryonsrelative to the cores produced in dark-matter-only runs, though the simulateddwarfs are always less centrally dense than in $\Lambda$CDM. TheV$_{1/2}-$r$_{1/2}$ relation across all simulations is generally consistentwith observations of Local Field dwarfs, though compact objects such as Tucanaprovide a unique challenge. Spatially-resolved rotation curves in the centralregions ($<400$ pc) of small dwarfs could provide a way to distinguish betweenCDM, WDM, and SIDM, however: at the masses probed in this simulation suite,cored density profiles in dwarfs with small r$_{1/2}$ values can only originatefrom dark matter self-interactions.

Dwarf Galaxies in CDM, WDM, and SIDM: Disentangling Baryons and Dark Matter Physics