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The dwarf planet Eris (2003 UB313, formerly known also as ``Xena'') is thelargest KBO up to now discovered. Despite being larger than Pluto and bearingmany similarities with it, it has not been possible insofar to detect anysignificant variability in its light curve, preventing the determination of itsperiod and axial ratio. We attempt to assess the level of variability of theEris light curve by determining its BVRI photometry with a target accuracy of0.03 mag/frame in R and a comparable or better stability in the calibration.Eris has been observed between November $30^\mathrm{th}$ and December$5^\mathrm{th}$ 2005 with the Y4KCam on-board the 1.0m Yale telescope at CerroTololo Interamerican Observatory, Chile in photometric nights. We obtain 7measures in B, 23 in V, 62 in R and 20 in I. Averaged B, V, and I magnitudes ascolors are in agreement within $\approx 0.03$ mag with measures from Rabinowitzet al. (2006) taken in the same nights. Night-averaged magnitudes in R shows astatistically significant variability over a range of about $0.05\pm0.01$ mag.This can not be explained by known systematics, background objects or someperiodical variation with periods less than two days in the light-curve. Thesame applies to B, V and to less extent to I due to larger errors. In analogywith Pluto and if confirmed by future observations, this ``long term''variability might be ascribed to a slow rotation of Eris, with periods longerthan 5 days, or to the effect of its unresolved satellite ``Dysnomea'' whichmay contribute for $\approx0.02$ mag to the total brightness.

Time series photometry of the dwarf planet ERIS (2003 UB313)