deletions | additions       diff --git a/section_Previous_measurements_citet_JIMMY13__.tex b/section_Previous_measurements_citet_JIMMY13__.tex  index 4901578..2c23da9 100644  --- a/section_Previous_measurements_citet_JIMMY13__.tex  +++ b/section_Previous_measurements_citet_JIMMY13__.tex 
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\section{Previous measurements}  \citet{JIMMY13} measured the stellar kinematics and photometry of the galaxies in our sample, we summarise their method and results in this section.  %-------------------------------------------------------------------------------------------------------------------  \subsection{Stellar Kinematics}\label{sec:ppxf} Kinematics}  First a signal-to-noise ratio (SNR) cut of 5 across all the spaxels (spatial pixels) was applied. The spaxels were then re-binned to a minimum SNR of 10, using the spatial binning Voronoi code of \citet{CAPPELLARI03}. The velocity and line-of-sight velocity dispersion were computed using the penalised fitting scheme of \citet[pPXF;][]{PPXF}, and the MILES \citep[Medium-resolution Isaac Newton Telescope Library of Empirical Spectra; ][]{MILES} library stellar templates. pPXF fits the stellar library templates to the absorption line features of the BCG spectra, giving the redshifts and the broadening of the spectral lines.  \\\\   \textbf{The angular momentum} was characterised by the $\lambda_{\rm R}$ parameter defined by \citet{EMSELLEM07}. It is calculated as follows:  
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\\\\  \textbf{The dynamical mass} was measured using the standard equation given in \citet{CAPPELLARI06}.   \begin{equation}\label{eq:mass} \begin{equation}  M_{dyn}=\frac{5R_e \sigma_e^2}{G},  \end{equation} 
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%------------------------------------------------------------------------------------------------------------------------------------------------------------------  \subsection{Photometric Analysis}  \citet{JIMMY13} analysed the photometry of this sample using images from SDSS Data Release 3. They measured the effective radius by fitting a 2D de Vaucouleurs profile. They also analysed the presence of recent mergers using the Gini, and M$_{\rm 20}$ coefficients \citep{LOTZ08}. This method studies the distribution of light looking for irregularities that could indicate morphological signatures of mergers. A galaxy is a merger candidate if it crosses the threshold:  \begin{equation}\label{eq:merger} \begin{equation}  G \geq -0.14M_{20} + 0.33  \end{equation}  Where M$_{\rm 20}$ is the 2nd order moment of the brightest 20~per~cent of pixels, and G is the Gini coefficient. In the case of gas-poor galaxies like our sample, a galaxy will be above the threshold if it is currently merging or has merged in the last 0.2~Gyr \citep{LOTZ11}. 4 of the BCGs in the sample are merging. The relevant kinematic and photometric results of \citet{JIMMY13} are presented in Table \ref{tab:kin}.