Table 1:

MLE fits to the radial distribution of the stacked halo.

Model			c
NFW	1	0	4.08  0.05  0.17	0.0021
NFW	1	(0.036)	4.10  0.05  0.17	0.0023
NFW	1	0.416	4.26  0.07  0.23	0.0069
Einasto	1	0	4.00  0.05  0.17	0.31
Einasto	1	(0.036)	4.02  0.05  0.17	0.3
Einasto	1	0.002	4.00  0.07  0.20	0.31
NFW	1.35	0	4.20  0.05  0.14	0.0023
NFW	1.35	(0.036)	4.23  0.05  0.14	0.0021
NFW	1.35	0.002	4.20  0.04  0.15	0.002
Einasto	1.35	0	4.14  0.04  0.13	0.016
Einasto	1.35	(0.036)	4.17  0.04  0.13	0.0058
Einasto	1.35	0.002	4.14  0.04  0.14	0.015
NFW	3	0	4.80  0.04  0.24	0
NFW	3	(0.036)	5.01  0.04  0.24	0
NFW	3	0.001	4.80  0.03  0.19	0
Einasto	3	0	4.26  0.03  0.22	<10-15
Einasto	3	(0.036)	4.50  0.03  0.23	<10-10
Einasto	3	0.042	4.54  0.04  0.13	<10-11

Notes. The Einasto models are for index m=5. Column (2) is the maximum radius for the fits (the minimum radius is set to 0.03 r₂₀₀). Columns (3) and (4) are respectively the background density (multiplied by 100, fixed if in parentheses) and concentration, while Col. (5) is the Kolmogorov-Smirnov test probability that the model is consistent with the distribution of radii. Virial units (with ) are used for and (r₂₀₀ and N₂₀₀/r₂₀₀², respectively), while c=r₂₀₀/r_-2, where r_-2 is the radius of density slope equal to -2. The outer radius of 1.35 r₂₀₀ corresponds to the virial radius, r₁₀₀. Errors are : the first are the statistical errors from likelihood ratios and the second are from cosmic variance using 100 cluster bootstraps. Concentrations in bold face are those providing the highest tests for given .