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We study a suite of extremely high-resolution cosmological FIRE simulationsof dwarf galaxies ($M_{\rm halo} \lesssim 10^{10}$$M_{\odot}$), run to $z=0$with $30 M_{\odot}$ resolution, sufficient (for the first time) to resolve theinternal structure of individual supernovae remnants within the cooling radius.Every halo with $M_{\rm halo} \gtrsim 10^{8.6} M_{\odot}$ is populated by aresolved {\em stellar} galaxy, suggesting very low-mass dwarfs may beubiquitous in the field. Our ultra-faint dwarfs (UFDs;$M_{\ast}<10^{5}\,M_{\odot}$) have their star formation truncated early($z\gtrsim2$), likely by reionization, while classical dwarfs ($M_{\ast}>10^{5}M_{\odot}$) continue forming stars to $z<0.5$. The systems have bursty starformation (SF) histories, forming most of their stars in periods of elevated SFstrongly clustered in both space and time. This allows our dwarf with$M_{\ast}/M_{\rm halo} > 10^{-4}$ to form a dark matter core $>200$pc, whilelower-mass UFDs exhibit cusps down to $\lesssim100$pc, as expected fromenergetic arguments. Our dwarfs with $M_{\ast}>10^{4}\,M_{\odot}$ havehalf-mass radii ($R_{\rm 1/2}$) in agreement with Local Group (LG) dwarfs;dynamical mass vs. $R_{1/2}$ and the degree of rotational support also resembleobservations. The lowest-mass UFDs are below surface brightness limits ofcurrent surveys but are potentially visible in next-generation surveys (e.g.LSST). The stellar metallicities are lower than in LG dwarfs; this may reflectpre-enrichment of the LG by the massive hosts or Pop-III stars. Consistencywith lower resolution studies implies that our simulations are numericallyrobust (for a given physical model).

Be it therefore resolved: Cosmological Simulations of Dwarf Galaxies with Extreme Resolution