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tokens: indicated by an arrow. We note, however, a group of six stars located within 2.6 core-radii of the center (red circles in Fig. 2 ) that show very similar kinematic properties, clustering around a mean velocity of km s. Likewise, as we will show in Sect. 4, their the metallicities are in excellent agreement with each other. While the presence of a secondary plume of stars at km s could in principle be identified with an underlying cluster population as well, these stars have markedly different metallicities (Sect. 4) and we rather deem these foreground objects. The same holds for those stars outside of the cluster boundary of , Thus we identify the innermost six stars at the higher velocity peak with members of FSR 1716. Their individual properties are listed in Table 2 . Table 2 Derived properties of the FSR 1716 member candidates. Thereby, we establish the mean systemic velocity of FSR 1716 as km s with a velocity dispersion of km s, a moderately low value typical of a low-to-intermediate mass Galactic star cluster (e.g., Pryor Meylan 1993 ; Koch et al. 2012 , 2017b ). Using this information and the cluster morphology in terms of its characteristic King (1966) radius ( Froebrich et al. 2008 ; Bonatto Bica 2008 ; Minniti et al. 2017 ), we can estimate the dynamical mass of FSR 1716 as ( Spitzer 1987 ), which is a factor of 70 larger than the low-mass estimate of Bonatto Bica (2008) , albeit based on their premise of a significantly lower distance. Upon a typical stellar mass-to-light ratio of 1.5, this would place FSR 1716 at an approximate absolute magnitude of mag, without doubt in the regimen of a GC. Ideally, the kinematic information should be coupled with accurate proper motions, allowing for an orbital computation that could hint at this cluster’s origin. Unfortunately, none of the member stars had a cross-match in the UCAC5 catalog ( Zacharias et al. 2017 ), and only three stars could be identified in the Hot Stuff for One Year (HSOY) proper motion catalog ( Altmann et al. 2017 ), which used the most recent positions from Gaia -DR1 ( Prusti et al. 2016 ). However, the respective proper motions are highly inconclusive, leading to a broad variety of possible orbits, from thick disk to outer halo; therefore, we do not pursue the orbital analyses any further. 4. Calcium triplet metallicities The three near-infrared CaT lines are a powerful indicator of stellar metallicities, [Fe/H], for RGB stars near and above the horizontal branch ( Armandroff Zinn 1988 ). In the following, we adopted the calibrations of line strength with metallicity from Vásquez et al. (2015) , which are applicable into the metal-rich regime up to 0.7 dex, and which employ the infrared magnitude above the red clump (). The latter is highly advantageous in population studies towards low latitudes, compared to the traditional use of the visual magnitude above the horizontal branch (), which is more sensitive to reddening. In practice, these calibrations are