Achromatic stellar interferometry

Details Achromatic stellar interferometry Achromatic stellar interferometry

Oct 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974optco..12..220c&link_type=abstract

Optics Communications, vol. 12, Oct. 1974, p. 220-222.

Physics

Optics

3

Diffraction Patterns, Interferometry, Michelson Interferometers, Stellar Radiation, Fourier Transformation, Luminous Intensity, Optical Filters, Signal To Noise Ratios, Telescopes

Scientific paper

One drawback of Michelson's stellar interferometer is due to the fact that the period of the interference fringes is proportional to the wavelength. Hence, in broadband light the fringe contrast is low, or in narrowband light (after filtering) the luminosity is low. We propose a modified stellar interferometer with perfectly achromatic fringes, that has better light efficiency and better signal to noise under most circumstances. To that end, two pieces of grating have to fill the two apertures of Michelson's setup. Achromatic interference fringes occur somewhere along the systems axis, where the plus-first diffraction order from one aperture meets the minus-first diffraction order from the other aperture. Laboratory experiments confirm the predicted achromatic performance.

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