Abstract
The beam combination scheme and the layout of the interferometer array determine the characteristics of the interferometer. If the reimaged telescope apertures in the beam combining instrument are a downscaled replica of the interferometer array, i.e. if they are mapped homothetically, the interferometer can be treated like a single telescope with a masked aperture, as discussed in Sect. 3.3.2, and the interferometric field of view is as large as that of the individual telescopes, limited by the optical design only. This is called theFizeau configuration, after Hippolyte Fizeau who was one of the first to publish the idea of stellar interferometry in 1868 [69].
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Notes
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- 2.
IOTA is the Infrared-Optical Telescope Array on Mt. Hopkins in Arizona, USA.
- 3.
PRIMA (Phase Referenced Imaging and Micro-arcsecond Astrometry) is the dual-feed facility of the VLTI.
- 4.
CHAMP was built for the CHARA interferometer on Mt. Wilson, California.
- 5.
CHARA is the Center for High Angular Resolution Astronomy at the Georgia State University, Georgia, USA.
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© 2011 Springer-Verlag Berlin Heidelberg
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Glindemann, A. (2011). Instrumental Techniques. In: Principles of Stellar Interferometry. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-15028-9_5
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DOI: https://doi.org/10.1007/978-3-642-15028-9_5
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