Detailed chemical composition and orbit of the new globular cluster
  FSR1758: Implications for the accretion of the Sequoia dwarf galaxy onto the
  Milky Way
  We present detailed chemical abundances, radial velocities and orbital
parameters for FSR 1758, a recently discovered star cluster in the direction of
the Galactic Bulge. High resolution (R~42,000) spectra were obtained using the
Magellan/Clay telescope instrumented with MIKE echelle spectrogragh, wavelength
range 4900-8700 \AA. Cluster membership was determined using Gaia DR2 proper
motions and confirmed with our radial velocity measurements. We find
metallicity consistent with previous photometric estimates for this cluster,
[Fe/H] = -1.58+-0.03 dex, with a small, 0.08 dex, spread. While other studies
have suggested this massive object may be the result of a previous accretion
event, our results are consistent with Milky Way Halo globular clusters with
characteristic Na-O anti-correlations found for the metal-poor cluster members.
The mean radial velocity of the cluster, +226.8+-1.6 km/s with a small velocity
dispersion, 4.9+-1.2 km/s, is typical for globular clusters. We also confirm a
retrograde Galactic orbit that appears to be highly eccentric.
