(2), including ν and σ F which typically are 0.5–0.7 mas. In this interval σ G is muchlarger than the other noise components in Eq. For the best-measured and generally brighter G ≃ −ġ8 stars with DR1 positional uncertaintiesof σ ∆. The residual RMS roughly matches the expectations given by the Gaia DR1 uncertainties, where we identified three regimesin terms of Gaia DR1 precision: for G ≃ −Ģ0 stars we found that the formal DR1 position uncertainties of stars with DR1 preci-sions in the range of 0.5–5 mas are underestimated by 63 ± −ġ0 mas areoverestimated by a factor of two. In the fields that we observed with FORS2, we projected the Gaia DR1 positions into the CCD plane, performed a polyno-mial fit between the two sets of matching stars, and carried out statistical analyses of the residuals in positions. The FORS2 position uncertainties are smaller than one milli-arcsecond (mas) andallowed us to perform an independent verification of the DR1 astrometric precision.
We compared positions of the Gaia first data release (DR1) secondary data set at its faint limit with CCD positions of stars in20 fields observed with the VLT / FORS2 camera. Sahlmann Main Astronomical Observatory, National Academy of Sciences of the Ukraine, Zabolotnogo 27, 03680 Kyiv, Ukrainee-mail: Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAReceived accepted
Gaia and VLT astrometry of faint stars: Precision of Gaia DR1positions and updated VLT parallaxes of ultracool dwarfs ⋆ P. A ug Astronomy&Astrophysicsmanuscript no. We also updated the FORS2 absolute parallax of the Luhman 16 binary brown dwarf system to 501.42 +/- 0.11 masĪa r X i v. By adopting Gaia DR1 as the absolute reference frame we refined the pixel scale determination of FORS2, leading to minor updates to the parallaxes of 20 ultracool dwarfs that we published previously. For the best-measured and generally brighter G = 16-18 stars with DR1 positional uncertainties of <0.5 mas, we detected 0.44 +/- 0.13 mas excess noise in the residual RMS, whose origin can be in both FORS2 and Gaia DR1. The residual RMS roughly matches the expectations given by the Gaia DR1 uncertainties, where we identified three regimes in terms of Gaia DR1 precision: for G = 17-20 stars we found that the formal DR1 position uncertainties of stars with DR1 precisions in the range of 0.5-5 mas are underestimated by 63 +/- 5\%, whereas the DR1 uncertainties of stars in the range 7-10 mas are overestimated by a factor of two. In the fields that we observed with FORS2, we projected the Gaia DR1 positions into the CCD plane, performed a polynomial fit between the two sets of matching stars, and carried out statistical analyses of the residuals in positions.
Astrometry rate across sky term verification#
The FORS2 position uncertainties are smaller than one milli-arcsecond (mas) and allowed us to perform an independent verification of the DR1 astrometric precision. We compared positions of the Gaia first data release (DR1) secondary data set at its faint limit with CCD positions of stars in 20 fields observed with the VLT/FORS2 camera.
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