The density profiles of Dark Matter halos in Spiral Galaxies

Understand

In spiral galaxies, we explain their non-Keplerian rotation curves (RCs) by means of a non-luminous component embedding their stellar-gaseous disks.

• Understanding the detailed properties of this component (labelled Dark Matter, DM) is one of the most pressing issues of Cosmology.
• We investigate the recent relationship (claimed by Walker et al.
• 2010, hereafter W+10) between $r$, the galaxy radial coordinate, and $V_h(r)$, the dark halo contribution to the circular velocity at $r$, {\it a}) in the framework of the Universal Rotation Curve (URC) paradigm and directly {\it b}) by means of the kinematics of a large sample of DM dominated spirals.