deletions | additions       diff --git a/sectionObservational.tex b/sectionObservational.tex  index e8365af..56c43e2 100644  --- a/sectionObservational.tex  +++ b/sectionObservational.tex 
...
The galaxy clusters selected to this work were extracted from the catalogue of 200 objects serendipitously detected in the ROSAT PSPC Pointed Observations (Vikhlinin et al. 1998) and the revised version by Mullis et al. (2003). The original catalogue contain galaxy clusters with X-ray lumiosities in the 0.5–2.0 keV energy band (observer frame), ranging from 10$^{42}$ to $\sim$ 50 $\times$ 10$^{43}$ erg s$^{−1}$ in the redshift range 0.16 to 0.70.   We define a sample consist in seven galaxy clusters, with intermediate X-ray luminosity (L$_X$ $\sim$ 0.5–45 $\times$ 10$^{43}$ erg s$^{−1}$), in the redshift range of 0.16 to 0.70. A complete description about the cluster observations can be found in Nilo Castell\'on et al. (2014A) (hereafeter paper 1). Mainly, the clusters were observed in the Gemini North and South Telescopes, using the Gemini Multi-Object Spectrograph (Hook et al. 2004, hereafter GMOS) in the image mode. The clusters were imaged through the \textit{r'} and \textit{g'} Sloan filters (Fukugita et al. 1996) under good photometric conditions with mean seeing values of 0.75, 0.66 and 0.74 arcsec in the \textit{g'} , \textit{r'} and \textit{i'} filters, respectively. Images were reduced using GEMINI/IRAF package, following the standard procedure. \citep{}. Table~\ref{tabla1} Table~\ref{table1}  shows a summary of the main characteristics of the clusters including the identification from Vikhlinin et al. (1998); the equatorial coordinates of the X-ray emission peak, the X-ray luminosity in the 0.5-2.0 keV energy band and also the mean redshift measured by Mullis et al. (2003) together with the Gemini Program identification and the observing passbands (including passbands, which include the  number of exposures and individual exposure time in seconds,respectively). seconds,respectively for each pass band.  \begin{table*}  \caption{Low X-ray luminosity Galaxy Clusters}  \label{table1}  {  \begin{tabular}{ccrrclccc}  \hline  \hline  [VMF98] & Right Ascension & Declination & $L_X$ &z & Program & g$^{\prime}$ & r$^{\prime}$ & i$^{\prime}$\\  Id. &(J2000) & (J2000) & [10$^{43}$ cgs] & & Id. & & & \\  \hline  & & & & & \\    001 & 00 30 33.2 & +26 18 19 & 26.1 & 0.500 & GN-2010B-Q-73 & -- & 15$\times$300 & 15$\times$150 \\  022 & 02 06 23.4 & +15 11 16 & 3.6 & 0.248 & GN-2003B-Q-10 & -- & 4$\times$300 & 4$\times$150 \\  093 & 10 53 18.4 & +57 20 47 & 1.4 & 0.340 & GN-2011A-Q-75 & -- & 5$\times$600 & 4$\times$150 \\  097 & 11 17 26.1 & +07 43 35 & 6.4 & 0.477 & GS-2003A-SV-206 & 12$\times$600 & 7$\times$900 & -- \\  119 & 12 21 24.5 & +49 18 13 & 42.7 & 0.700 & GN-2011A-Q-75 & -- & 7$\times$190 & 4$\times$120 \\  124 & 12 52 05.4 & -29 20 46 & 3.4 & 0.188 & GS-2003A-SV-206 & 5$\times$300 & 5$\times$600 & -- \\  148 & 13 42 49.1 & +40 28 11 & 16.2& 0.699 & GN-2011A-Q-75 & --& 7$\times$190 & 5$\times$120 \\  & & & & & \\   \hline  \hline  \end{tabular}  }  \end{table*}