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5 31(190), 256–259 (1891a). 1080/14786449108620101. tandfonline. A. Michelson, XXXVIII. On the application of interference-methods to spectroscopic measurements. Philos. Mag. Ser. 5 31(191), 338–346 (1891b). 1080/14786449108620117. 1080/14786449108620117 F. Millour, All you ever wanted to know about optical long baseline stellar interferometry, but were too shy to ask your adviser. New Astron. Rev. D. Monnier, Optical interferometry in astronomy. Rep. Prog. Phys. 66(5), 789 (2003). H. Norton, R.
1 m away from the source (the focal length of the reflector) to generate a flat wavefront for the interferometer. 027 deg/mm. 5 mm; (iii) a third aperture being identical to the second with one of the slits covered with a low-pass filter (edge at 21 cm−1 ). The third aperture is used to have a different source not only spatially, but also spectrally. As the interferometer is only sensitive in one spatial dimension, the slits are arranged perpendicular to the projected scanning direction to increase the overall signal available.
Suppl. 15(1974), 417–426 (1974) K. Itoh, Y. Ohtsuka, Fourier-transform spectral imaging: retrieval of source information from threedimensional spatial coherence. J. Opt. Soc. Am. A 3(1), 94–100 (1986). 3. 000094. R. T. J. B. J. L. G. A. H. Teng, X. Zhang, in Wide-field imaging interferometry testbed I: purpose, testbed design, data, and synthesis algorithms, ed. by M. Shao. Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, vol. 4852 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series (2003), pp.