Colour − magnitude diagrams for the newly observed GGC in our sample. Grey dots show our pre-imaging V, V − I photometry, calibrated with literature data (see text). For 47 Tuc, which was not part of our original observations, we used the photometry by Rosenberg et al. (2000). A selection on the photometric parameters from DAOPHOT II is applied to show only the best measured stars. Black dots mark spectroscopic targets. Clusters are ordered as a function of their metallicity from the most metal-poor (top left) to the most metal-rich (bottom right).