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Low surface brightness galaxies are an excellent laboratory where stars andbaryonic matter act as tracers of the gravitational potential of the darkmatter halo. If dark matter is modeled as a perfect fluid, then sphericallysymmetric and static dark matter halos in hydrostatic equilibrium demand thatdark matter should have an intrinsic pressure that counteracts thegravitational attraction that the dark matter halo exerts on itself. Thisstatic fluid (dark matter-dominated system, where the presence of baryons isnegligible) has a specific equation of state for each rotational velocityprofile of the stars in galaxies. In this work, we study the dark matterequation of state needed for the self-gravitating object to produce agravitational potential such that the tracers follow the Universal RotationalVelocity Profile for stars of spiral galaxies proposed by Persic et al. (1996)and analyze the properties of the self-gravitating structures that emerge fromthis equation of state.The resulting configurations explaining the observedrotational speeds are found to be unstable. We conclude that the halo is not inhydrostatic equilibrium, it is nonspherically symmetric, or it is not static ifthe universal velocity profile should be valid for fitting the rotationalvelocity curve of the galaxies.

Preliminary Study on Dark Matter-Dominated Systems: Further Analysis for galactic dark matter halos with Pressure