  Recent studies show that the inner Galactic regions host genuine bulge
globular clusters, but also halo intruders, complex remnants of primordial
building blocks, and objects likely accreted during major merging events. In
this study we focus on the properties of M 28, a very old and massive cluster
currently located in the Galactic bulge. We analysed wide-field infrared
photometry collected by the VVV survey, VVV proper motions, and
intermediate-resolution spectra in the calcium triplet range for 113 targets in
the cluster area. Our results in general confirm previous estimates of the
cluster properties available in the literature. We find no evidence of
differences in metallicity between cluster stars, setting an upper limit of
Delta[Fe/H]<0.08 dex to any internal inhomogeneity. We confirm that M 28 is one
of the oldest objects in the Galactic bulge (13-14 Gyr). From this result and
the literature data, we find evidence of a weak age-metallicity relation among
bulge globular clusters that suggests formation and chemical enrichment. In
addition, wide-field density maps show that M 28 is tidally stressed and that
it is losing mass into the general bulge field. Our study indicates that M 28
is a genuine bulge globular cluster, but its very old age and its mass loss
suggest that this cluster could be the remnant of a larger structure, possibly
a primeval bulge building block.
