Local tests of GR and reference frames linking with GAIA astrometry of asteroids

Details Local tests of GR and reference frames linking with GAIA astrometry of asteroids Local tests of GR and reference frames linking with GAIA astrometry of asteroids

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jsrs.meet..133h&link_type=abstract

"Proceedings of the "Journées Systèmes de Référence Spatio-temporels 2007". Observatoire de Paris, 17-19 September 2007. Editor:

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Scientific paper

The Gaia satellite, an ESA cornerstone mission to be launched at the end of the year 2011, will observe a large number of celestial bodies including also small bodies of the solar system (mainly near-Earth objects and main-belt asteroids). The scanning telescope will observe all objects brighter than magnitude V ≤ 20 providing, over the 5 years mission, high precision photometry and astrometry with an unprecedented accuracy ranging roughly from ≈ 0.3 to 3 milli-arcsecond on the CCD level, and depending on the target’s magnitude. In addition, several hundreds of QSOs directly observed by Gaia will provide the kinematically non-rotating reference frame in the visible light, resulting in the construction of a ’Gaia-ICRF’. The positions of the asteroids hence enable to relate the dynamical reference frame as defined by the equations of motions to the kinematic one, and to further check the non-rotating consistency between both frames definition. Here we show the results of a variance analysis obtained from a realistic simulation of observations for such link. The simulation takes into account the time sequences and geometry of the observations that are particular to Gaia observations of solar system objects, as well as the instrument sensitivity and photon noise. Additionally, we show the achievable ˙ precision for the determination of a possible time variation of the gravitational constant G/G. Taking into account the non-completeness of the actually known population of NEOs, we also give updated values for the nominal precision of the joint determination of the solar quadrupole J2 and PPN parameter β. Comparison to the results obtained from other techniques is also given.

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