We study the total and dark matter ( DM ) density profiles as well as their correlations for a sample of 15 high-mass galaxy clusters by extending our previous work on several clusters from Newman et al .
Our analysis focuses on 15 CLASH X-ray-selected clusters that have high-quality weak- and strong-lensing measurements from combined Subaru and Hubble Space Telescope observations .
The total density profiles derived from lensing are interpreted based on the two-phase scenario of cluster formation .
In this context , the brightest cluster galaxy ( BCG ) forms in the first dissipative phase , followed by a dissipationless phase where baryonic physics flattens the inner DM distribution .
This results in the formation of clusters with modified DM distribution and several correlations between characteristic quantities of the clusters .
We find that the central DM density profiles of the clusters are strongly influenced by baryonic physics as found in our earlier work .
The inner slope of the DM density for the CLASH clusters is found to be flatter than the Navarro–Frenk–White profile , ranging from \alpha = 0.30 to 0.79 .
We examine correlations of the DM density slope \alpha with the effective radius R _ { \mathrm { e } } and stellar mass M _ { \mathrm { e } } of the BCG , finding that these quantities are anti-correlated with a Spearman correlation coefficient of \sim - 0.6 .
We also study the correlation between R _ { \mathrm { e } } and the cluster halo mass M _ { 500 } , and the correlation between the total masses inside 5 kpc and 100 kpc .
We find that these quantities are correlated with Spearman coefficients of 0.68 and 0.64 , respectively .
These observed correlations are in support of the physical picture proposed by Newman et al .