The present paper is an extension and continuation of Del Popolo ( 2012a ) which studied the role of baryon physics on clusters of galaxies formation .
In the present paper , we studied by means of the SIM introduced in Del Popolo ( 2009 ) , the total and DM density profiles , and the correlations among different quantities , observed by Newman et al .
( 2012a , b ) , in seven massive and relaxed clusters , namely MS2137 , A963 , A383 , A611 , A2537 , A2667 , A2390 .
As already found in Del Popolo 2012a , the density profiles depend on baryonic fraction , angular momentum , and the angular momentum transferred from baryons to DM through dynamical friction .
Similarly to Newman et al .
( 2012a , b ) , the total density profile , in the radius range 0.003 - 0.03 r _ { 200 } , has a mean total density profile in agreement with dissipationless simulations .
The slope of the DM profiles of all clusters is flatter than -1 .
The slope , \alpha , has a maximum value ( including errors ) of \alpha = -0.88 in the case of A2390 , and minimum value \alpha = -0.14 for A2537 .
The baryonic component dominates the mass distribution at radii < 5 - 10 kpc , while the outer distribution is dark matter dominated .
We found an anti-correlation among the slope \alpha , the effective radius , R _ { e } , and the BCG mass , and a correlation among the core radius r _ { core } , and R _ { e } .
Moreover , the mass in 100 kpc ( mainly dark matter ) is correlated with the mass inside 5 kpc ( mainly baryons ) .

The behavior of the total mass density profile , the DM density profile , and the quoted correlations can be understood in a double phase scenario .
In the first dissipative phase the proto-BCG forms , and in the second dissipationless phase , dynamical friction between baryonic clumps ( collapsing to the center ) and the DM halo flattens the inner slope of the density profile .

In simple terms , the large scatter in the inner slope from cluster to cluster , and the anti-correlation among the slope , \alpha and R _ { e } is due to the fact that in order to have a total mass density profile which is NFW-like , clusters having more massive BCGs at their centers must contain less DM in their center .
Consequently the inner profile has a flatter slope .