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\section{Observational Dataset:}  \label{sec:data}   The clusters studied analize  in this paper are selected from the sample of nineteen low X-ray luminosity  galaxy clusters studied by Nilo Castellon et al (2014A) (hereafter paper I). The authors create a photometric and spectroscopic data base with 19 low and intermediate X-ray luminosities galaxy clusters in the redshift range of 0.15 to 0.70 and observed X-ray luminosities between L$_X$$\sim$ L$_X$\sim$  0.5-45 $\times$10${43}$ erg s−1. The clusters were observed in 4 diferent observatories across the world, observatories,  according to their redshift: clusters at z < 0.32 were observed at Las Campanas Observatory (LCO) using the 2.5m du Pont telescope, clusters at 0.19 < z < 0.30 were observed at the Cerro Tololo Interamerican Observatory (CTIO) using the Victor Blanco 4m telescope telescope,  andfinally  clusters at z>0.3 were observed with Gemini North (GN) and South (GS) telescopes. Also, three clusters at z<0.3 were observed with the 8mts  Gemini telescopes in order to observed the faintest galaxies in each these  cluster (for further details see Paper I). The study of the faintest detections in the images is a major concern in our work. work ({\bf algo por el estilo quiero agregar}).  In order to this, we select a subsample of 7 galaxy clusters, all of them observed with the Gemini North and South telescopes. the clusters were observed using the Multi-Object Spectrograph (Hook et al. 2004, hereafter GMOS) in the image mode, with $g\prime$, $r\prime$ and $i\prime$ filters. All the observations were carried under good and excelente photometric conditions with mean seeing values of 0.75, 0.66 and 0.74 arcsec in the$g\prime$, $r\prime$ and $i\prime$ filters, respectively. Reaching in the case of the cluster [VMF98]001, median seeing of about 0.485 in the $r\prime$ image (For forther details about the observation strategy see Nilo Castellon et al. (2014B)). All the observations were reduced using standard procedures in IRAF1 (Tody 1993) and specific packages, depending on  the instruments and telescopes utilised. The images were overscanned and bias subtracted, trimmed and flat-fielded following the standard reduction procedures. Individual images were put into a common po sition system and then combined to create final images.