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In this section we summarise the observations made and the data reduction process. These are described in full in \citet{JIMMY13}.   %------------------------------------------------------------------------------------------------------------------------------------------------------------------   \subsection{Spectroscopic Measurements}\label{sec:obs}  The BCG sample is selected from \citet{LINDEN07}. The galaxies are part of the C4 cluster catalogue (Miller 2005) of the third data release of the Sloan Digital Sky Survey \citep[SDSS; ][]{YORK00}. These observations consist of 10 BCGs, 4 of which have massive companions within $\sim 10^{\prime\prime}$ 10$arcsec  (corresponding to $\sim 18$~kpc at $z<0.1$). We use the same nomenclature as \citet{JIMMY13}, i.e. we present each cluster as the last 4 digits in the SDSS flag, rather than SDSS-C4-DR3 \textit{number}. The galaxies were observed with the Very Large Telescope using the IFU mode of the VIMOS spectrograph \citep[][]{LEFEVRE03}, with the high-resolution blue grism, which has a spectral resolution of 0.51~\AA/pixel. The observations were made in two sets, April to August of 2008 and April to July of 2011 (Prog.~ID 381.B-0728 and Prog.~ID 087.B-0366, respectively). The galaxies used in this study have a spatial sampling of $0.67^{\prime\prime}$/pixel $0.67arcsec$/pixel  with a field-of-view (FOV) of $27^{\prime\prime} $27arcsec  \times 27^{\prime\prime}$. 27arcsec$.  The average seeing of the observations is $0.9^{\prime\prime}$. $0.9arc$.  The rest wavelength range is $\sim3900$~to~$5600$~\AA. %------------------------------------------------------------------------------------------------------------------------------------------------------------------  \subsection{IFU Data Reduction}\label{sec:redu}  The IFU data reduction consists of two different stages: (a) The VIMOS Pipeline \citep{IZZO04} which generates the calibrations files (fibre identification, master bias, etc.), and does a first order flux calibration. This flux calibration corrects the spectrum shape, using the standard stars observed on the same night as the galaxies. The VIMOS FOV is formed by four quadrants. The VIMOS pipeline reduces each quadrant separately. As a result we obtain the science spectrum for each spaxel in each quadrant. (b) We use our own IDL routines to mask the bad fibres, subtract the sky for each quadrant and then combine the quadrants into a three dimensional data cube. The multiple exposures for each observation are combined using a 5$\sigma$ clipped median. This code is publicly available\footnote{http://galaxies.physics.tamu.edu/index.php/Jimmy\#Code}. Finally, we flux calibrate the spectrum using the photometric standard stars.