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

Free access article

Issue		A&A Volume 460, Number 2, December III 2006


Page(s)		L39 - L42
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:20066526

A&A 460, L39-L42 (2006)
DOI: 10.1051/0004-6361:20066526

Letter

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

G. Carraro^{1, 2}, M. Maris³, D. Bertin², and M. G. Parisi^{2, 4}

¹ Dipartimento di Astronomia, Università di Padova, Vicolo Osservatorio 2, 35122 Padova, Italy
e-mail: gcarraro@das.uchile.cl
² Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
³ INAF, Osservatorio Astronomico di Trieste, via Tiepolo 11, 40013 Trieste, Italy
⁴ Facultad de Ciencias Astronómicas y Geofísicas de la UNLP, IALP-CONICET, Paseo del Bosque s/n, La Plata, Argentina

(Received 9 October 2006 / Accepted 19 October 2006 )

Abstract
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 30th and December 5th, 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 $\approx$ 0.03 mag 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 $0.05\pm0.01$ mag. 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.
Conclusions. 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 5 days, or to the effect of its unresolved satellite "Dysnomea", which may contribute for $\approx$ 0.02 mag to the total brightness.

Key words: Kuiper Belt -- solar system: general -- minor planets, asteroids -- techniques: photometric

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