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

Autores
Carraro, G.; Maris, M.; Bertin, D.; Parisi, Mirta Gabriela
Año de publicación
2006
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
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 ≈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.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Kuiper Belt
Minor planets, asteroids
Solar system: general
Techniques: photometric
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/83253

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network_name_str SEDICI (UNLP)
spelling Time series photometry of the dwarf planet ERIS (2003 UB313)Carraro, G.Maris, M.Bertin, D.Parisi, Mirta GabrielaCiencias AstronómicasKuiper BeltMinor planets, asteroidsSolar system: generalTechniques: photometric<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.Facultad de Ciencias Astronómicas y Geofísicas2006-11-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfL39-L42http://sedici.unlp.edu.ar/handle/10915/83253enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066526info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:15:45Zoai:sedici.unlp.edu.ar:10915/83253Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:15:45.962SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Time series photometry of the dwarf planet ERIS (2003 UB313)
title Time series photometry of the dwarf planet ERIS (2003 UB313)
spellingShingle Time series photometry of the dwarf planet ERIS (2003 UB313)
Carraro, G.
Ciencias Astronómicas
Kuiper Belt
Minor planets, asteroids
Solar system: general
Techniques: photometric
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)
dc.creator.none.fl_str_mv Carraro, G.
Maris, M.
Bertin, D.
Parisi, Mirta Gabriela
author Carraro, G.
author_facet Carraro, G.
Maris, M.
Bertin, D.
Parisi, Mirta Gabriela
author_role author
author2 Maris, M.
Bertin, D.
Parisi, Mirta Gabriela
author2_role author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Kuiper Belt
Minor planets, asteroids
Solar system: general
Techniques: photometric
topic Ciencias Astronómicas
Kuiper Belt
Minor planets, asteroids
Solar system: general
Techniques: photometric
dc.description.none.fl_txt_mv <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.
Facultad de Ciencias Astronómicas y Geofísicas
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.
publishDate 2006
dc.date.none.fl_str_mv 2006-11-03
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/83253
url http://sedici.unlp.edu.ar/handle/10915/83253
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6361
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066526
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
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rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
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