The imaging process in stellar interferometers is explained
starting from first principles on wave propagation and diffraction.
Wave propagation through turbulence is described in detail using
Kolmogorov statistics. The impact of turbulence on the imaging
process is discussed both for single telescopes and for
interferometers. Correction methods (adaptive optics and fringe
tracking) are presented including wavefront sensing/fringe sensing
methods and closed loop operation. Instrumental techniques like
beam combination and visibility measurements (modulus and phase) as
well as Nulling and heterodyne interferometry are described. The
book closes with examples of observing programmes linking the
theory with individual astrophysical programmes.
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