2006A&A...460L..39C

The dwarf planet Eris (2003 UB313, formerly known also as ``Xena'') is the largest KBO discovered up to now. Despite being larger than Pluto and having many similarities to it, it has not been possible so far to detect any significant variability in its light curve, preventing the determination of its period and axial ratio. We attempt to assess the level of variability of the Eris light curve by determining its BVRI photometry with a target accuracy of 0.03mag/frame in R and a comparable or better stability in the calibration. Eris has been observed between November 30th and December 5th, 2005 with the Y4KCam onboard the 1.0m Yale telescope at Cerro Tololo Interamerican Observatory, Chile in photometric nights. We obtain 7 measures in B, 23 in V, 62 in R, and 20 in I. Averaged B, V, and I magnitudes as colors are in agreement within ≃0.03mag with measures from Rabinowitz et al. (2006, [arXiv:astro-ph/0605745]) taken on the same nights. Night-averaged magnitudes in R show a statistically significant variability over a range of about 0.05±0.01mag. This cannot be explained by known systematics, background objects, or some periodical variation with periods less than two days in the lightcurve. The same applies to B, V and to a lesser extent to I, due to larger errors. In analogy with Pluto and if confirmed by future observations, this ``long term'' variability might be ascribed to a slow rotation of Eris, with periods longer than 5days, or to the effect of its unresolved satellite ``Dysnomea'', which may contribute for ≃0.02mag to the total brightness.