Dark matter densities in cluster isochrones

We found that, when a cluster is surrounded by a dense DM halo, the positions of the cluster' stars in the H-R diagram have a brighter and hotter turnoff point than in the classical scenario without DM, therefore giving the cluster a younger appearance.

The high DM densities required to produce these effects are expected only in very specific locations, such as near the center of our Galaxy. In particular, if DM is formed by the 8 GeV weakly interacting massive particles recently invoked to reconcile the results from direct detection experiments, then this signature is predicted for halos of DM with a density {rho}_{chi}_=3x10^5^GeV/cm^3^. A DM density gradient inside the stellar cluster would result in a broader main sequence, turnoff, and red giant branch regions.