Confirming the intrinsic abundance spread in the globular cluster NGC
  6273 (M 19) with calcium triplet spectroscopy
  We present metallicities for red giant stars in the globular cluster NGC 6273
based on intermediate resolution GMOS-S spectra of the calcium triplet region.
For the 42 radial velocity members with reliable calcium triplet line strength
measurements, we obtain metallicities, [Fe/H], using calibrations established
from standard globular clusters. We confirm the presence of an intrinsic
abundance dispersion identified by Johnson et al. (2015). The total range in
[Fe/H] is ~1.0 dex and after taking into account the measurement errors, the
intrinsic abundance dispersion is \sigma[Fe/H] = 0.17 dex. Among the Galactic
globular clusters, the abundance dispersion in NGC 6273 is only exceeded by
omega Cen, which is regarded as the remnant of a disrupted dwarf galaxy, and M
54, which is the nuclear star cluster of the Sagittarius dwarf galaxy. If these
three globular clusters share the same formation mechanism, then NGC 6273 may
also be the remnant nucleus of a disrupted dwarf galaxy.
