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Paola Oliva-Altamirano added section_Conclusions_We_present_the__.tex
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\section{Conclusions}
We present the first analysis of the stellar populations of 9 BCGs using IFU observations. We compare their stellar populations to those of the IFU observations of field early-type galaxies from the SAURON and ATLAS$^{3D}$ sample. We draw the following conclusions:
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(1) The BCGs have a wide range of stellar ages, high metallicities, and have shallow metallicity gradients. This implies diverse evolutionary paths (passive and active accretion). The BCGs' central stellar populations and gradients are consistent with those of early-type galaxies of similar mass, with the exception that the BCGs have a wide range of central ages.
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(2) Three of the BCGs have similar mass close companions galaxies within 18~kpc. From those 3 BCGs we were able to resolve the companions of 2 of them. The companion galaxies have central stellar populations consistent with their respective BCG.
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(3) We do not observe a relationship between the stellar populations of BCGs and their stellar kinematics (slow and fast rotators).
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IFU analysis has allowed us to determine the angular momentum of BCGs and to study their stellar population gradients without the orientation bias innate to long-slit spectroscopy. It has also allowed us to include their companion galaxies in the analysis. This study hints of intriguing differences between BCGs and similar mass early-type galaxies but requires much larger samples to confirm. The SAMI galaxy survey \citep{FORGARTY14, ALLEN14} currently underway will allow us to achieve this goal. New ultra wide-field IFU spectrographs such as MUSE on the Very Large Telescope and large date sets as the MASSIVE survey \citep[][]{MA14} will also allow us to determine whether the picture is different at radii beyond 1~R$_e$.
