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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 observation observations  can be found in Nilo Castell\'on et al. (2014A) (hereafeter paper 1). Mainlly, 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{}.\\ \citep{}. Table~\ref{tabla1} 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 num-  ber of exposures and individual exposure time in seconds,  respectively).  The galaxy population for our clusters of galaxies sample was extensively analized in paper II \citep{}, At redshift > 0.4 a less important Red Cluster Sequence with a smaller extension was found compared against the low redshift sample, but with a clear presence of the blue population. The total galaxy radial density profiles were well fitted by a single power law. For the three galaxy clusters with spectroscopic measurements, no significant detection of substructures through the Dressler Shectman Test \citep{} analysis was found.  The fractions of elliptical, lenticular and blue galaxies