Astron. Astrophys. Suppl. Ser.
Volume 121, Number 3, March 1997
|Page(s)||553 - 568|
|Published online||15 March 1997|
Correction of the “piston effect” in optical astronomical interferometry
I. Modulus and phase gradient of the visibility function restoration
Observatoire de Paris, DESPA, 5 place Jules Janssen, F-92195 Meudon, France
Send offprint request to: G. Perrin
Accepted: 7 November 1996
An a posteriori method to cancel out atmospheric optical path fluctuations to achieve accurate phase restoration and spectral analysis of interferograms is presented in this paper. The correction algorithm is based on classical noise reduction methods. The consequence of piston noise is twofold: 1) loss of spectral information; 2) loss of visibility phase. A method to measure the modulus and the phase gradient of visibilities is explained and examples of restoration of simulated spectra and visibilities for various ratios are presented.
Key words: atmospheric effects / methods: data analysis / technics: interferometric
© European Southern Observatory (ESO), 1997