Abstract

I am developing an approach to astrometry in which controlled motion of the star field is used to convert the troublesome spatial metric into the more easily measurable temporal metric. The Multi-Anode Microchannel Array (MAMA) detector is ideally suited to this project because of its geometrical stability and the precise timing information it provides. In a rudimentary observational test using the Kitt Peak National Observatory 4-Meter Mayall Telescope, the precision obtained was consistent with the ideal limit based on photon statistics and the assumption that no systematic errors are present. The availability of precise arrival times for each detected photon opens up fascinating possibilities for innovations in the data analysis, including post-facto compensation for atmospheric seeing effects. New techniques for the determination of star-image centroids are described below.

© 1983 Optical Society of America