Astrometric planet search around southern ultracool dwarfs

Abstract

We present an investigation of the stability of the two chips in the FORS2 camera CCD mosaic on the basis of astrometric observations of stars in 20 sky fields, some of which were monitored for four to seven years. We detected a smooth relative shear motion of the chips along their dividing line that is well approximated by a cubic function of time with an amplitude that reaches ∼0.3 pixels (px) or ∼38 mas over seven years. In a single case, we detected a step change of ∼0.06 px that occurred within four days. In the orthogonal direction that corresponds to the separation between the chips, the motion is a factor of 5–10 smaller. This chip instability in the camera significantly reduces the astrometric precision when the reduction uses reference stars located in both chips, and the effect is not accounted for explicitly. We found that the instability introduces a bias in stellar positions with an amplitude that increases with the observation time span. When our reduction methods and FORS2 images are used, it affects stellar positions like an excess random noise with an rms of ∼0.5 mas for a time span of three to seven years when left uncorrected. We demonstrate that an additional calibration step can adequately mitigate this and restore an astrometric accuracy of 0.12 mas, which is essential to achieve the goals of our planet-search program. These results indicate that similar instabilities could critically affect the astrometric performance of other large ground-based telescopes and extremely large telescopes that are equipped with large-format multi-chip detectors if no precautions are taken.

Individual dynamical masses of DENIS J063001.4−184014AB reveal a likely young brown dwarf triple

“…2 OBSERVATIONS AND DATA REDUCTION 2.1 Very Large Telescope/FORS2 astrometry Here we do not present new FORS2 measurements, but we improve the accuracy of prior measurements by accounting for the updated camera calibrations presented in Lazorenko & Sahlmann (2017) and Lazorenko & Sahlmann (2019). These improvements include the use of Gaia catalogues (Gaia Collaboration et al 2016) for external astrometric calibration and accounting for the subtle changes in the camera's CCD chip locations.…”

“…We derived an RMS of 4 mas for the 'FORS2-DR2' difference in positions, which exceeds its expected value of about 1 mas. Such a large RMS value is probably due to the different scale and relative rotation of the chips in the FORS2 detector, which was not introduced in the transformation model whereas the difference in zero points was taken into account as discussed in Lazorenko & Sahlmann (2019).…”