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\subsection{Stellar populations from the SAURON and ATLAS$^{3D}$ samples}\label{sec:sauron}
Throughout the paper we compare our observations to those of early-type galaxies of similar mass observed by ATLAS$^{3D}$ (which includes the SAURON galaxy sample). The ATLAS$^{3D}$ sample is composed of 260 field and cluster early-type galaxies and it only contains one BCG, M87. The spatially-resolved stellar populations (central values and gradients) of the SAURON sample were presented in \citet{KUNTSCHNER10}. The central stellar populations of the ATLAS$^{3D}$ sample were presented in \citet{ATLAS3D}. We therefore compare our central stellar populations with the whole ATLAS$^{3D}$ sample and the stellar population gradients only with the SAURON sample.
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\citet{KUNTSCHNER10} and \citet{ATLAS3D} use the stellar models of \citet{SCHIAVON07} in the Lick/IDS system \citep{WORTHEY97} to measure the stellar population parameters of age, total metallicity [Z/H] and abundance of alpha elements [$\alpha$/Fe]. For our spectral fitting, we use models with only solar abundances, i.e. $[\alpha$/Fe$]=0$. In this case [Fe/H] is effectively a measure of the total metallicity\footnote{[Fe/H] = [Z/H] - 0.75*[$\alpha$/Fe] \citep{CONROY12} }. Therefore, we directly compare the ATLAS$^{3D}$ total metallicities to our measured metallicities throughout the paper. The central stellar populations in the ATLAS$^{3D}$ sample correspond to an aperture of 0.125~R$_e$.
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We compare the median, and standard deviation for the two samples in the same mass range (M$_{dyn}>10^{11.3}$M$_{\odot}$). In order to compare our BCGs with a non-BCG early-type galaxy sample, we do not include the BCG M87. This gives a comparison sample of 20 massive early-type galaxies from the ATLAS$^{3D}$ sample. We highlight M87 as a blue-filled circle in the figures.
