@Article{CamargoMVABDBGAS:2015:18YeOb,
author = "Camargo, J. I. B. and Magalh{\~a}es, Fab{\'{\i}}ola Pinho and
Vieira-Martins, R. and Assafin, M. and Braga-Ribas, F. and
Dias-Oliveira, A. and Benedetti-Rossi, G. and Gomes-J{\'u}nior,
A. R. and Andrei, A. H. and Silva Neto, D. N.",
affiliation = "{Observat{\'o}rio Nacional (ON)} and {Instituto Nacional de
Pesquisas Espaciais (INPE)} and {Observat{\'o}rio Nacional (ON)}
and {Observat{\'o}rio Do Valongo} and {Observat{\'o}rio Nacional
(ON)} and {Observat{\'o}rio Nacional (ON)} and {Observat{\'o}rio
Nacional (ON)} and {Observat{\'o}rio Do Valongo} and
{Observat{\'o}rio Nacional (ON)} and {Centro Universit{\'a}rio
Estadual da Zona Oeste}",
title = "Astrometry of the main satellites of Uranus: 18 years of
observations",
journal = "Astronomy \& Astrophysics",
year = "2015",
volume = "582",
pages = "A8",
month = "Oct.",
keywords = "Astrometry, Catalogs, Methods: data analysis, Planets and
satellites: individual: Uranus.",
abstract = "Context. We contribute to developing dynamical models of the
motions of Uranus' main satellites. Aims. We determine accurate
positions of the main satellites of Uranus: Miranda, Ariel,
Umbriel, Titania, and Oberon. Positions of Uranus, as derived from
those of these satellites, are also determined. The observational
period spans from 1992 to 2011. All runs were made at the Pico dos
Dias Observatory, Brazil. Methods. We used the software called
Platform for Reduction of Astronomical Images Automatically
(PRAIA) to perform a digital coronography to minimise the
influence of the scattered light of Uranus on the astrometric
measurements and to determine accurate positions of the main
satellites. The positions of Uranus were then indirectly
determined by computing the mean differences between the observed
and ephemeris positions of these satellites. A series of numerical
filters was applied to filter out spurious data. These filters are
mostly based on (a) the comparison between the positions of Oberon
with those of the other satellites and on (b) the offsets as given
by the differences between the observed and ephemeris positions of
all satellites. Results. We have, for the overall offsets of the
five satellites,-29 mas (±63 mas) in right ascension and-27 mas
(±46 mas) in declination. For the overall difference between the
offsets of Oberon and those of the other satellites, we have +3
mas (±30 mas) in right ascension and-2 mas (±28 mas) in
declination. Ephemeris positions for the satellites were
determined from DE432+ura111. Comparisons using other modern
ephemerides for the solar system-INPOP13c-and for the motion of
the satellites-NOE-7-2013-were also made. They confirm that the
largest contribution to the offsets we find comes from the motion
of the barycenter of the Uranus system around the barycenter of
the solar system, as given by the planetary ephemerides. For the
period from 1992 to 2011, our final catalogues contain 584
observed positions of Miranda, 1710 of Ariel, 1987 of Umbriel,
2588 of Titania, 2928 of Oberon, and 3516 of Uranus.",
doi = "10.1051/0004-6361/201526385",
url = "http://dx.doi.org/10.1051/0004-6361/201526385",
issn = "0004-6361 and 1432-0746",
language = "en",
targetfile = "2015_camargo.pdf",
urlaccessdate = "27 abr. 2024"
}