too bright and were saturated in the deeper $RIZ$ images. We choose to include all the above objects as likely cluster members.

Colour magnitude diagrams for the X-ray sources with cluster counterparts are shown in Figs. \[vbvcmd\], \[vvicmd\] and \[iricmd\]. A distance of 417 pc, $E(B-V)=0.06$, $E(V-I)=0.077$ and $E(R-I)=0.043$ were assumed (see Jeffries & Oliveira 2005 and references therein). Cluster candidates that lie within 15 arcminutes of the [*XMM-Newton*]{} pointing and which were [*not*]{} detected as X-ray sources are shown for comparison. Details of the X-ray sources with cluster counterparts are given in Tables \[xraymembers\] and \[counterparts\]. The number of spurious correlations was estimated by applying random 30 arcsecond offsets to the X-ray sources. From these tests fewer than 2 of the 108 cluster X-ray sources are expected to be spurious correlations. X-ray sources are detected from across the mass range covered by the cluster members. For low-mass objects our census is limited by the sensitivity of the X-ray observations (see section 4.1). The faintest detected cluster members have $V\simeq 19.5$ and $I\simeq 16.5$, corresponding to about 0.25$M_{\odot}$ from the isochrones used in Figs. \[vvicmd\] and \[iricmd\]. The observations are not sensitive enough (by a factor of a few) to 