quadrature to the X-ray astrometric uncertainties in order to yield a reduced $\chi^{2}$ of unity in the fit to the mean offset of 38 bright X-ray/cluster-object correlations. This additional error corresponds perfectly with the expected precision of the current [*XMM-Newton*]{} attitude reconstruction (Kirsch et al. 2005). In stage 2 this offset and additional error were applied and the full X-ray source list correlated with the membership catalogues using an error circle of radius 3 times the total positional error. 103 correlations were found between $BVI$ selected members and X-ray sources and 67 correlations between $RIZ$ selected members and X-ray sources. There are a total of 108 X-ray sources with a cluster counterpart, 5 of which were not considered members by Naylor et al. (2002) using $BVI$ photometry (they look just too blue in $B-V$) and 8 of which are not considered members by Jeffries et al. (2004) using $RIZ$ photometry (3 look just too blue in the $R-I$ vs $I-Z$ diagram and 5 lie a little too far above the cluster isochrone in $I$ vs $R-I$). A further 33 objects that are members in the $BVI$ catalogue have no good photometry in the $RIZ$ catalogue, mostly because these stars are 