Homogeneous metallicities and radial velocities for Galactic globular clusters ^⋆,⋆⋆

II. New CaT metallicities for 28 distant and reddened globular clusters

¹ Museo Interactivo Mirador, Dirección de Educación, Av. Punta Arenas 6711, La Granja, Santiago, Chile
² European Southern Observatory, Alonso de Córdova 3107, Santiago, Chile
³ INAF – Osservatorio Astronomico di Padova, vicolo Osservatorio 5, 35122 Padova, Italy
e-mail: enrico.held@oapd.inaf.it
⁴ Research School of Astronomy & Astrophysics, Australian National University, Mt Stromlo Observatory, via Cotter Rd, Weston, ACT 2611, Australia
⁵ Universidade de São Paulo, Rua do Matão 1226, São Paulo 05508-900, Brazil
⁶ Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, vicolo dell’Osservatorio 3, 35122 Padova, Italy
⁷ Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Santiago, Chile
⁸ Millennium Institute of Astrophysics, Av. Vicuña Mackenna 4860, Santiago, Chile

Received: 29 May 2018
Accepted: 25 July 2018

Abstract

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 ∼69% of those listed in the Harris’ catalogue. As in our previous work, we have used the Ca II 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 Ca II 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 Ca II 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.