Detailed Chemical Composition and Orbit of the Newly Discovered Globular Cluster FSR 1758: Implications for the Accretion of the Sequoia Dwarf Galaxy onto the Milky Way Based on observations carried out at the Magellan/Clay telescope under program CN2018B-71

• Published in: The Astrophysical journal 2019-09, Vol.882 (2)
• Main Authors: Villanova, Sandro, Monaco, Lorenzo, Geisler, Doug, O'Connell, Julia, Minniti, Dante, Assmann, Paulina, Barbá, Rodolfo
• Format: Article
• Language: English
• Subjects: Globular star clusters
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ab3722

We present detailed chemical abundances, radial velocity, and orbital parameters for FSR 1758, a recently discovered massive cluster in the direction of the Galactic bulge. High-resolution (R ∼ 42,000) spectra were obtained for nine members using the Magellan/Clay telescope instrumented with the MIKE echelle spectrogragh in the wavelength range of ∼4900-8700 . Cluster membership was determined using Gaia DR2 proper motions and confirmed with our radial velocity measurements. We find a metallicity of [Fe/H] = −1.58 0.03, consistent with previous photometric estimates, and no significant iron spread. While other studies have suggested that this massive object could be the remnant of a captured dwarf galaxy, our results are consistent with a globular cluster (GC) nature, given its lack of any intrinsic metallicity spread and the Na-O anticorrelation similar to those of other GC. In addition, the small velocity dispersion of 4.9 1.2 km s−1 we find is that typical of a GC. We also confirm a retrograde orbit that appears to be highly eccentric suggesting it is a halo interloper currently in the bulge. We support the hypothesis that FSR 1758 was part of a disrupted dwarf galaxy named Sequoia.