Open AccessRotational effects in the system of proper motions of the UCAC3 catalogue
Author(s) -
Bobylev V. V.,
Khovritchev M. Yu.
Publication year - 2011
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2011.19389.x
Subject(s) - physics , stars , proper motion , galaxy , astrophysics , reference frame , astrometry , spherical harmonics , rotation (mathematics) , formalism (music) , astronomy , frame (networking) , geometry , art , telecommunications , musical , mathematics , quantum mechanics , computer science , visual arts
A set of ≈8 million single stars of the UCAC3 catalogue has been analysed. It contains stars with reliable proper motions with not less than three epochs of observations used to compute the proper motion. Our main goal is to investigate the inertiality of the reference system defined by ‘good’ stars of the UCAC3 catalogue. The formalism of vectorial spherical harmonics has been applied to analyse the system of proper motions of the selected UCAC3 stars. A comparison between the results of solutions for several subsets of UCAC3 stars shows that the key parameters significantly change with stellar magnitudes, colours and average distances. The values of the components of the rigid‐body rotation vector of the Hipparcos Celestial Reference Frame (HCRF) with respect to extragalactic sources were determined using ‘proper motions’ of more than 8000 galaxies of the UCAC3 catalogue. The values are ω 1 = 0.58 ± 0.15, ω 2 =−1.02 ± 0.15, ω 3 =−0.59 ± 0.17 mas yr −1 in galactic coordinates. Traces of the considerable magnitude equation are seen in the ‘proper motions’ of the UCAC3 galaxies. The most significant component derived from the analysis of the UCAC3 galaxies is ω 2 . It does not contradict the results of the analysis of the proper motions of selected stars (ω 2 =−1.09 ± 0.02 mas yr −1 ).