tokens: by Binggeli et al. ( 1985 ) in the Virgo Cluster Catalog (VCC), although no redshift has been published. Indeed, Binggeli et al. ( 1985 , p. 1756) classified VCC 1287 as a dwarf irregular galaxy “ .. of very large size and low surface brightness. ” GCs were identified exploiting all five MegaCam bands. A catalog of sources was extracted using SExtractor (Bertin Arnouts 1996 ). Only objects detected in all five bands were considered, selecting point sources by imposing the i -band class star parameter of SExtractor to be >0.5. This removes most extended objects from the catalog, owing to the excellent (06) seeing of the images. We selected as GC candidates all point sources within the following color ranges: 0.6 ( g − z ) 1.2, 1.1 ( u − g ) 1.8, and 0.7 ( g − i ) 1.0. We selected a fairly narrow color range in order to minimize contamination from background sources (in particular, red background galaxies). However, these color ranges are consistent with the distributions seen in other studies of Virgo dwarf galaxies (e.g., Beasley et al. 2006 ; Peng et al. 2006 ). In order to exclude ultra-compact galaxies, we also imposed a magnitude cut, i > 19.5 mag, equivalent to the magnitude of the Milky Way GC ω Cen at the distance of Virgo. To determine the total number of GCs in VCC 1287, we constructed the surface density profile of the GC system and found it to extend to ∼175′′ (∼13 kpc), beyond which is a constant background with 0.2 objects per arcmin 2 . Next, all point sources within 175′′ of the galaxy center and that satisfy our selection criteria were flagged as GCs—returning 18 candidates. Star and galaxy contamination were calculated by the random placement of 1000 circles with 175′′ radii in the 1 deg 2 field surrounding VCC 1287. We found a mean of 6 objects expected within such a circle, with a standard deviation of 2.5 counts using our selection criteria, with no sky apertures with 18 objects. The identification of 18 GC candidates represents an overdensity with respect to the background level at ∼5 σ significance. Subtracting this contamination rate left 11 GC candidates down to the GC turnover magnitude ( i = 23.1, using I -band values of Kundu Whitmore 2001 and an i -band transformation from Faifer et al. 2011 ). Assuming that the GC luminosity function is bell-shaped (Harris et al. 2000 ), we doubled their number to obtain a total GC population of 22 ± 8 GCs, where the uncertainties come from the quadrature sum of the Poisson uncertainties and the background contribution. This may not sound remarkable, but when normalized to the host galaxy magnitude using the “specific frequency” ( S N ; Harris van den Bergh 1981 ), we find VCC 1287 has S N = 80 ± 29. This is a significant overabundance of GCs for VCC 1287's stellar luminosity (Figure 4 ). 2.2. GC Spectroscopy GC candidates were selected for multi-object spectroscopy with the OSIRIS instrument on the Gran Telescopio de Canarias (GTC) in La Palma. We observed this spectroscopic
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