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

<b>Context.</b> 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 curv...

Descripción completa

Guardado en:
Detalles Bibliográficos
Autores principales: Carraro, G., Maris, M., Bertin, D., Parisi, Mirta Gabriela
Formato: Articulo
Lenguaje:Inglés
Publicado: 2006
Materias:
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/83253
Aporte de:
id I19-R120-10915-83253
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Kuiper Belt
Minor planets, asteroids
Solar system: general
Techniques: photometric
spellingShingle Ciencias Astronómicas
Kuiper Belt
Minor planets, asteroids
Solar system: general
Techniques: photometric
Carraro, G.
Maris, M.
Bertin, D.
Parisi, Mirta Gabriela
Time series photometry of the dwarf planet ERIS (2003 UB313)
topic_facet Ciencias Astronómicas
Kuiper Belt
Minor planets, asteroids
Solar system: general
Techniques: photometric
description <b>Context.</b> 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. <b>Aims.</b> 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. <b>Methods.</b> 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. <b>Results.</b> 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/0605745]) taken on the same nights. Night-averaged magnitudes in R show a statistically significant variability over a range of about 0.05 ± 0.01 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 ≈0.02 mag to the total brightness.
format Articulo
Articulo
author Carraro, G.
Maris, M.
Bertin, D.
Parisi, Mirta Gabriela
author_facet Carraro, G.
Maris, M.
Bertin, D.
Parisi, Mirta Gabriela
author_sort Carraro, G.
title Time series photometry of the dwarf planet ERIS (2003 UB313)
title_short Time series photometry of the dwarf planet ERIS (2003 UB313)
title_full Time series photometry of the dwarf planet ERIS (2003 UB313)
title_fullStr Time series photometry of the dwarf planet ERIS (2003 UB313)
title_full_unstemmed Time series photometry of the dwarf planet ERIS (2003 UB313)
title_sort time series photometry of the dwarf planet eris (2003 ub313)
publishDate 2006
url http://sedici.unlp.edu.ar/handle/10915/83253
work_keys_str_mv AT carrarog timeseriesphotometryofthedwarfplaneteris2003ub313
AT marism timeseriesphotometryofthedwarfplaneteris2003ub313
AT bertind timeseriesphotometryofthedwarfplaneteris2003ub313
AT parisimirtagabriela timeseriesphotometryofthedwarfplaneteris2003ub313
bdutipo_str Repositorios
_version_ 1764820488433958914