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

Context. 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. Aims. We attempt to assess the level of variability of the Eris light curve by determining its BVRI photometry with a target accuracy of 0.03 mag/frame in R and a comparable or better stability in the calibration. Methods.Eris has been observed between November $30\mathrm{th}$ and December $5\mathrm{th}$, 2005 with the Y4KCam onboard the 1.0 m Yale telescope at Cerro Tololo Interamerican Observatory, Chile in photometric nights. Results. 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 ≈$ 0.03$ mag with measures from Rabinowitz et al. (2006, [arXiv:astro-ph/060574