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In this work we model galactic halos describing the dark matter as a non zeropressure fluid and derive, not impose, a dark matter equation of state by usingobservational data of the rotation curves of galaxies. In order to reachhydrostatic equilibrium, as expected for the halo, it is mandatory that darkfluid's pressure should not be zero. The equation of state is obtained bysolving the matter-geometry system of equations assuming different dark matterdensity or rotational velocity profiles. The resulting equations of state are,in general, different to a barotropic equation of state. The free parameters ofthe equation of state are fixed by fitting the observed rotational velocitiesof a set of galaxies.

Dark matter equation of state from rotational curves of galaxies