  Although the globular clusters in the Milky Way have been studied for a long
time, a significant fraction of them lack homogeneous metallicity and radial
velocity measurements. In an earlier paper we presented the first part of a
project to obtain metallicities and radial velocities of Galactic globular
clusters from multiobject spectroscopy of their member stars using the ESO Very
Large Telescope. In this paper we add metallicities and radial velocities for a
new sample of 28 globular clusters, including in particular globular clusters
in the MW halo and the Galactic bulge. Together with our previous results, this
study brings the number of globular clusters with homogeneous measurements to
$\sim 69$ \% of those listed in the W. Harris' catalogue. As in our previous
work, we have used the CaII triplet lines to derive metallicities and radial
velocities. For most of the clusters in this study, this is the first analysis
based on spectroscopy of individual member stars. The metallicities derived
from the CaII triplet are then compared to the results of our parallel study
based on spectral fitting in the optical region and the implications for
different calibrations of the CaII triplet line strengths are discussed. We
also comment on some interesting clusters and investigate the presence of an
abundance spread in the globular clusters here. A hint of a possible intrinsic
spread is found for NGC 6256, which therefore appears to be a good candidate
for further study.
