Interferometric data reduction with AMBER/VLTI.Principle,estimators and illustration

Details Interferometric data reduction with AMBER/VLTI.Principle,estimators and illustration Interferometric data reduction with AMBER/VLTI.Principle,estimators and illustration

2006-03-02

arxiv.org/abs/astro-ph/0603046v1

Astronomy and Astrophysics

Astrophysics

16 pages, 10 figures. Accepted in A&A

Scientific paper

10.1051/0004-6361:20064799

We present in this paper an innovative data reduction method for single-mode interferometry. It has been specifically developed for the AMBER instrument, the three-beam combiner of the Very Large Telescope Interferometer, but can be derived for any single-mode interferometer. The algorithm is based on a direct modelling of the fringes in the detector plane. As such, it requires a preliminary calibration of the instrument in order to obtain the calibration matrix which builds the linear relationship between the interferogram and the interferometric observable, that is the complex visibility. Once the calibration procedure has been performed, the signal processing appears to be a classical least square determination of a linear inverse problem. From the estimated complex visibility, we derive the squared visibility, the closure phase and the spectral differential phase. The data reduction procedures are gathered into the so-called amdlib software, now available for the community, and presented in this paper. Furthermore, each step of this original algorithm is illustrated and discussed from various on-sky observations conducted with the VLTI, with a focus on the control of the data quality and the effective execution of the data reduction procedures. We point out the present limited performances of the instrument due to VLTI instrumental vibrations, difficult to calibrate.

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