Wide-angle astrometry with the Mark III stellar interferometer

Details Wide-angle astrometry with the Mark III stellar interferometer Wide-angle astrometry with the Mark III stellar interferometer

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aj....100.1701s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 100, Nov. 1990, p. 1701-1711.

Astronomy and Astrophysics

Astronomy

18

Angular Resolution, Astrometry, Interferometers, Wide Angle Lenses, Accuracy, Data Reduction, Error Analysis, Gratings (Spectra), Seeing (Astronomy)

Scientific paper

Astrometric measurements made with the Mark III stellar interferometer on five nights in August-September 1988 yielded average formal 1-sigma errors for 12 FK5 stars of 6 mas in declination and 10 mas in right ascension. This improvement in precision over previously reported measurements with this instrument made in 1986 is attributable to several factors: a second 12 m baseline; oriented E-S, was added to the instrument to improve the determination of right ascension; two-color analysis was included in the data-reduction process, along with a new central-fringe identification algorithm using three spectral channels, in order to reduce atmospheric errors; thermal control was greatly improved; and changes were made to observational procedures and hardware to monitor variations in the delay offset due to residual thermal drifts. Approximately half of the new positions are within 50 mas of their FK5 positions. However, an extended series of measurements are needed to ascertain the accuracy that can be achieved by interferometry.

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