PROCEEDINGS ARTICLE | July 22, 2010
Proc. SPIE. 7734, Optical and Infrared Interferometry II
KEYWORDS: Telescopes, Stars, Interferometers, Image restoration, Interferometry, Computer simulations, Space telescopes, Gamma radiation, Atmospheric Cherenkov telescopes, Device simulation
Kilometric-scale optical imagers seem feasible to realize by intensity interferometry, using telescopes primarily
erected for measuring Cherenkov light induced by gamma rays. Planned arrays envision 50-100 telescopes, distributed
over some 1-4 km2. Although array layouts and telescope sizes will primarily be chosen for gamma-ray
observations, also their interferometric performance may be optimized. Observations of stellar objects were numerically
simulated for different array geometries, yielding signal-to-noise ratios for different Fourier components
of the source images in the interferometric (u, v)-plane. Simulations were made for layouts actually proposed for
future Cherenkov telescope arrays, and for subsets with only a fraction of the telescopes. All large arrays provide
dense sampling of the (u, v)-plane due to the sheer number of telescopes, irrespective of their geographic orientation
or stellar coordinates. However, for improved coverage of the (u, v)-plane and a wider variety of baselines (enabling better image reconstruction), an exact east-west grid should be avoided for the numerous smaller telescopes, and repetitive geometric patterns avoided for the few large ones. Sparse arrays become severely limited by a lack of short baselines, and to cover astrophysically relevant dimensions between 0.1-3 milliarcseconds in visible wavelengths, baselines between pairs of telescopes should cover the whole interval 30-2000 m.
