A method to analyze adaptive optics images of binary stars

Details A method to analyze adaptive optics images of binary stars A method to analyze adaptive optics images of binary stars

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26as..135..187b&link_type=abstract

Astronomy and Astrophysics Supplement, v.135, p.187-195

Physics

Optics

Stars: Tau Canis Majoris, Instrumentation, Adaptive Optics, Techniques: Image Processing

Scientific paper

We present a fast and robust ad-hoc method to analyze a set of short exposure images of a close binary star taken by the adaptive optics system of the ESO 3.6 m telescope. At first each image is fitted, assuming as a radially symmetrical approximation of its ``instantaneous'' PSF, the superposition of a central Gaussian and of a Moffat torus. Owing to the coral variability and asymmetry of the PSF the fit gives a poor estimate of the component's luminosity ratio; nevertheless it reproduces satisfactorily the global structure of the PSF and above all gives the accurate sub-pixel positions of the two stars. This allows to obtain, by the shift-and-add procedure, the mean set image from which the final parameters of the two stars and the mean PSF during the observing run are derived. The results from a set of AO images of the close binary system tau Canis Maioris are consistent with those previously obtained by one of us using the iterative blind deconvolution. Extensive simulations give evidence that the magnitude difference and the separation of the components can be estimated within about 0.05 mag and 0\farcs005 respectively when the secondary star image does not overlap a bright artifact of the AO system.

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