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In an attempt to place an explicit constraint on dark matter models, wedefine and estimate a mean surface density of a dark halo within a radius ofmaximum circular velocity, which is derivable for various galaxies with anydark-matter density profiles. We find that this surface density is generallyconstant across a wide range of maximum circular velocities of $\sim$ 10 to 400km s$^{-1}$, irrespective of different density distribution in each of thegalaxies. This common surface density at high halo-mass scales is found to benaturally reproduced by both cold and warm dark matter (CDM and WDM) models,even without employing any fitting procedures. However, the common surfacedensity at dwarf-galaxy scales, for which we have derived from the Milky Wayand Andromeda dwarf satellites, is reproduced only in a massive range of WDMparticle masses, whereas CDM provides a reasonable agreement with the observedconstancy. This is due to the striking difference between mass-concentrationrelations for CDM and WDM halos at low halo-mass scales. In order to explainthe universal surface density of dwarf-galaxy scales in WDM models, we suggestthat WDM particles need to be heavier than 3 keV.

A common surface-density scale for the Milky Way and Andromeda dwarf satellites as a constraint on dark matter models