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We report spectroscopic observations with the Gemini South Telescope of 5faint V~20 RR Lyrae stars associated with the Pisces overdensity. At aheliocentric and galactocentric distance of ~80 kpc, this is the most distantsubstructure in the Galactic halo known to date. We combined our observationswith literature data and confirmed that the substructure is composed of twodifferent kinematic groups. The main group contains 8 stars and has <V_{gsr}> =50 km/s, while the second group contains four stars at a velocity of <V_{gsr}>= -52 km/s, where V_{gsr} is the radial velocity in the galactocentric standardof rest. The metallicity distribution of RR Lyrae stars in the Piscesoverdensity is centered on [Fe/H]=-1.5 dex and has a width of 0.3 dex. The newdata allowed us to establish that both groups are spatially extended making itvery unlikely that they are bound systems, and are more likely to be debris ofa tidally disrupted galaxy or galaxies. Due to small sky coverage, it is stillunclear whether these groups have the same or different progenitors.

Halo Velocity Groups in the Pisces Overdensity