\begin{table}%t1 
\caption{\label{c3d}MLE fits to the radial distribution of the stacked halo.}
\small%\centering
\par
\begin{tabular}{lllcl}
\hline\hline\noalign{\smallskip}
Model & $r_{\rm max}$ & \multicolumn{1}{c}{$100~\hat\nu_{\rm bg}$} & $c$ & \multicolumn{1}{c}{$P_{\rm KS}$} \\
\noalign{\smallskip}\hline
NFW & 1 & 0 & 4.08~$\pm$~0.05~$\pm$~0.17 & 0.0021\\ 
NFW & 1 & (0.036) & 4.10~$\pm$~0.05~$\pm$~0.17 & 0.0023\\ 
NFW & 1 & 0.416 & 4.26~$\pm$~0.07~$\pm$~0.23 & 0.0069\\ 
Einasto & 1 & 0 & {\bf 4.00~$\pm$~0.05~$\pm$~0.17} & 0.31\\ 
Einasto & 1 & (0.036) & 4.02~$\pm$~0.05~$\pm$~0.17 &  0.3\\ 
Einasto & 1 & 0.002 & 4.00~$\pm$~0.07~$\pm$~0.20 & 0.31\\ 
NFW & 1.35 & 0 & 4.20~$\pm$~0.05~$\pm$~0.14 & 0.0023\\ 
NFW & 1.35 & (0.036) & 4.23~$\pm$~0.05~$\pm$~0.14 & 0.0021\\ 
NFW & 1.35 & 0.002 & 4.20~$\pm$~0.04~$\pm$~0.15 & 0.002\\ 
Einasto & 1.35 & 0 & {\bf 4.14~$\pm$~0.04~$\pm$~0.13} & 0.016\\ 
Einasto & 1.35 & (0.036) & 4.17~$\pm$~0.04~$\pm$~0.13 & 0.0058\\ 
Einasto & 1.35 & 0.002 & 4.14~$\pm$~0.04~$\pm$~0.14 & 0.015\\ 
NFW & 3 & 0 & 4.80~$\pm$~0.04~$\pm$~0.24 &    0\\ 
NFW & 3 & (0.036) & 5.01~$\pm$~0.04~$\pm$~0.24 &    0\\ 
NFW & 3 & 0.001 & 4.80~$\pm$~0.03~$\pm$~0.19 &    0\\ 
Einasto & 3 & 0 & 4.26~$\pm$~0.03~$\pm$~0.22 & $<$$10^{-15}$\\
Einasto & 3 & (0.036) & {\bf 4.50~$\pm$~0.03~$\pm$~0.23} &  $<$$10^{-10}$\\
Einasto & 3 & 0.042 & 4.54~$\pm$~0.04~$\pm$~0.13 & $<$$10^{-11}$\\ 
\hline
\end{tabular} 
\tablefoot{The Einasto models are for index $m=5$. Column~(2) is the maximum
radius for the fits (the minimum radius 
is set to $0.03~r_{200}$). 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 $\Delta=200$) are used for $r_{\rm max}$ and $\hat\nu_{\rm
  bg}$ ($r_{200}$ and 
$N_{200}/r_{200}^2$, respectively), while $c=r_{200}/r_{-2}$, where
$r_{-2}$ is the radius of density slope equal to $-2$. The outer radius of
$1.35~r_{200}$ 
corresponds to the virial radius, $r_{100}$.
Errors are $1\sigma$: 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 $P_{\rm KS}$
tests for given $r_{\rm max}$.}
\end{table}