An updated survey of globular clusters in M 31 . II . Newly discovered bright and remote clusters

Aims. We present the first results of a large spectroscopic survey of candidate globular clusters located in the extreme outskirts of the nearby M31 galaxy. The survey is aimed at ascertaining the nature of the selected candidates to increase the sample of confirmed M31 clusters lying more that 2 • away from the center of the galaxy. Methods. We obtained low resolution spectra (λ/∆λ ≃ 800 − 1300) of 48 targets selected from the Extended Source Catalogue of 2MASS, as in Galleti et al. (2005). The observed candidates have been robustly classified according to their radial velocity and by verifying their extended/point-source nature from ground-based optical images. We have also obtained a spectrum and a radial velocity estimate for the remote M31 globular discovered by Martin et al. (2006b). Results. Among the 48 observed candidates clusters we found: 35 background galaxies, 8 foreground Galactic stars, and 5 genuine remote globular clusters. One of them has been already identified independently by Mackey et al. (2007), their GC1; the other four are completely new discoveries: B516, B517, B518, B519. The newly discovered clusters lie at projected distance 40 kpc < ∼ R p < ∼ 100 kpc from the center of M31, and have absolute integrated magnitude −9.5 < ∼ M V < ∼ − 7.5. For all the observed clusters we have measured the strongest Lick indices and we have obtained spectroscopic metallicity estimates. Mackey-GC1, Martin-GC1, B517 and B518 have spectra typical of old and metal poor globular clusters ([Fe/H] < ∼ − 1.3); B519 appears old but quite metal-rich ([Fe/H]≃ −0.5); B516 presents very strong Balmer absorption lines: if this is indeed a cluster it should have a relatively young age (likely < 2 Gyr). Conclusions. The present analysis nearly doubles the number of M31 globulars at R p ≥ 40 kpc. At odds with the Milky Way, M31 appears to have a significant population of very bright globular clusters in its extreme outskirts.