VizieR Online Data Catalog: APOGEE southern GCs with the BACCHUS code (Meszaros+, 2020)

Our target selection follows that of Meszaros et al. (2015AJ....149..153M, Cat. J/AJ/149/153) and Masseron et al. (2019A&A...622A.191M, Cat. J/A+A/622/A191). We select stars based on their radial velocity first, their distance from cluster centre second, and their metallicity third. In radial velocity, we required stars to be within three times the velocity dispersion of the mean cluster velocity, and in distance we required stars to be within the tidal radius. The metallicity cut was usually set to +/-0.5dex around the cluster average, except for clusters with suspected intrinsic Fe spread for which the metallicity cut was skipped, or only obvious field stars were deleted (for example, stars with solar-like metallicity in otherwise metal-poor clusters). For this paper we made important updates by selecting the average cluster radial velocity and its scatter from Gaia DR2 (Baumgardt & Hilker 2018MNRAS.478.1520B, Cat. J/MNRAS/478/1520) rather than from Harris (1996AJ....112.1487H, Cat. VII/195, 2010 edition). In addition, we introduced a fourth step that is based upon selecting stars that have proper motion within a 1.5-2.5mas/yr range (depending on the cluster) around the cluster average proper motion from the Gaia DR2 catalogue (Gaia Collaboration 2018A&A...616A...1G, Cat. I/345).

The individual atmospheric parameters and the derived abundances are listed in Table 2, while the abundance averages and RMS scatters for each cluster are presented in Table 3. Table 2 contains results for all stars and clusters that were analysed, altogether 3382 stars in 44 clusters.

(2 data files).