The retrograde orbit of the globular cluster FSR1758 revealed with Gaia DR2

Abstract

We report the first radial velocity measurements of the recently identified globular cluster FSR1758. From the two member stars with radial velocities from the Gaia Radial Velocity Spectrograph reported in Gaia DR2, we find FSR1758 has a radial velocity of $227\pm 1$ km/s. We also find potential extra-tidal star lost from the cluster in the surrounding 1~deg. Combined with Gaia proper motions and photometric distance estimates, this shows that FSR1758 is on a very retrograde, radial orbit with an pericentre of $3.8_{-0.9}^{+0.9}$ kpc, an apocentre of $16_{-5}^{+8}$ kpc, and eccentricity of $0.62_{-0.04}^{+0.05}$. Although it is currently at a Galactocentric distance of $3.8_{-0.9}^{+0.9}$ kpc --- at the edge of the bulge --- it is an intruder from the halo. We investigate whether a reported `halo' of stars around FSR1758 is related to the cluster, and find that most of these stars are likely foreground dwarf stars. We conclude that FSR1758 is not a dwarf galaxy, but rather a globular cluster.

6 pages, 4 figures, 1 table. Accepted for publication in MNRAS. Refereed version has one fewer member stars that submitted version. Data and code for producing figures is available from https://doi.org/10.5281/zenodo.2550945

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• Blanco DECam Bulge Survey (BDBS) II: Project Performance, Data Analysis, and Early Science Results
• Probing the Galactic Halo with RR Lyrae Stars. II. The Substructures of the Milky Way
• CAPOS: the bulge Cluster APOgee Survey II. The Intriguing "Sequoia" Globular Cluster FSR 1758
• On the Origin of the Globular Cluster FSR 1758
• Milky Way globular cluster dynamics: are they preferentially co-rotating?