Volume 582, October 2015
|Number of page(s)||12|
|Section||Catalogs and data|
|Published online||29 September 2015|
1 Observatório Nacional/MCTI, R. General José Cristino 77, CEP 20921-400, Rio de Janeiro, RJ, Brazil
2 Laboratório Interinstitucional de e-Astronomia – LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil
3 Instituto Nacional de Pesquisas Espaciais, Av. dos Astronautas 1758, CEP 12227-010 São José dos Campos, SP, Brazil
4 Affiliated researcher at the Observatoire de Paris/IMCCE, 77 av. Denfert-Rochereau, 75014 Paris, France
5 Observatório do Valongo/UFRJ, Ladeira do Pedro Antônio 43, CEP 20080-090 Rio de Janeiro, RJ, Brazil
6 Associated researcher at the Observatoire de Paris/IMCCE, 77 av. Denfert-Rochereau, 75014 Paris, France
7 Federal University of Technology – Paraná (UTFPR / DAFIS), Rua Sete de Setembro, 3165 CEP 80230-901, Curitiba, PR, Brazil
8 Associated researcher at the Observatoire de Paris/SYRTE, 77 av. Denfert Rochereau, 75014 Paris, France
9 Associated researcher at the INAF/Osservatorio Astronomico di Torino, Strada Osservatorio 20, 10025 Pino Torinesi (To), Italy
10 Centro Universitário Estadual da Zona Oeste, Av. Manual Caldeira de Alvarenga 1203, CEP 23. 070-200 Rio de Janeiro RJ, Brazil
Received: 22 April 2015
Accepted: 24 July 2015
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.
Key words: astrometry / methods: data analysis / catalogs / planets and satellites: individual: Uranus
Tables with the positions of Uranus and its satellites, as well as with the X and Y CCD coordinates of the observed satellites and reference stars are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/582/A8
© ESO, 2015
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