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We present zoom-in N-body + Hydrodynamic simulations of dwarf centralgalaxies formed in Warm Dark Matter (WDM) halos with masses at present-day of$2-4\times 10^{10}$ \msun. Two different cases are considered, the first onewhen halo masses are close to the corresponding half-mode filtering scale \Mhm\(\mwdm =1.2 keV), and the second when they are 20 to 30 times the corresponding\Mhm\ (\mwdm = 3.0 keV). The WDM simulations are compared with the respectiveCold Dark Matter (CDM) simulations. The dwarfs formed in halos of masses(20-30)\Mhm have roughly similar properties and evolution than their CDMcounterparts; on the contrary, those formed in halos of masses around \Mhm, aresystematically different from their CDM counterparts. As compared to the CDMdwarfs, they assemble the dark and stellar masses later, having mass-weightedstellar ages 1.4--4.8 Gyr younger; their circular velocity profiles areshallower, with maximal velocities 20--60% lower; their stellar distributionsare much less centrally concentrated and with larger effective radii, byfactors 1.3--3. The WDM dwarfs at the filtering scale (\mwdm =1.2 keV) havedisk-like structures, and end in most cases with higher gas fractions and lowerstellar-to-total mass ratios than their CDM counterparts. The late haloassembly, low halo concentrations, and the absence of satellites of the formerwith respect to the latter, are at the basis of the differences.

Simulations of galaxies formed in warm dark matter halos of masses at the filtering scale