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Beam Combination for Wide Field Imaging

Published online by Cambridge University Press:  19 July 2016

M. Tallon  and
I. Tallon-Bosc
M. Tallon
Affiliation:
URA CNRS 709, Dpt. d'Astrophysique, Université de Nice, F-06108 Nice cedex 2
I. Tallon-Bosc
Affiliation:
URA CNRS 1361, Observatoire de la Côte d'Azur, F-06460 Saint-Vallier de Thiey

Abstract

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Several limitations reduce the field of view in radio-interferometry. With an optical array, two of them can be overcome to some extent according to the beam combination method. A beam combination in the pupil plane can completely overcome one of them. In the image plane, a beam combination obeying the rules of geometrical optics can overcome both limitations in principle, but is difficult to achieve in practice. We discuss particularly the real case of a Michelson Stellar Interferometer where a periscope partially re-introduces these limitations, yielding a trade-off between the extension of the field of view and the use of the periscope.

Type
Imaging Techniques
Information
Symposium - International Astronomical Union , Volume 158: Very High Angular Resolution Imaging , 1994 , pp. 83 - 90
Copyright
Copyright © Kluwer 1994 

References

[1] VLT report 65: 1992, “Coherent combined instrumentation for the VLT Interferometer”, ESO Ed., Garching, F.R.G. Google Scholar
[2] Born, M. and Wolf, E.: 1980, “Principles of Optics”, Pergamon Press, New York Google Scholar
[3] Coudé du Foresto, V.: 1993, this conference.Google Scholar
[4] Cornwell, T. J. and Perley, R. A.: 1992, Astron. Astrophys. 261, 353.Google Scholar
[5] Tallon, M. and Tallon-Bosc, I.: 1992, Astron. Astrophys. 253, 641.Google Scholar
[6] Schwab, F. R.: 1984, AJ 89, 1076.Google Scholar
[7] Mariotti, J.-M.: 1990, SPIE 1237, p647 Google Scholar
[8] Bryngdahl, O. and Lohmann, A.: 1970, Appl. Opt. 9, 231.CrossRefGoogle Scholar
[9] Stephan, H.: 1874, C. R. Acad. Sc. Paris 78, 1008.Google Scholar
[10] Meinel, A. B.: 1970, Appl. Opt. 9, 2501.Google Scholar
[11] Beckers, J. M., Hege, E. K. and Strittmatter, P. A.: 1983, SPIE 444, p85.Google Scholar
[12] Weaver, L. D., Fender, J. S. and De Hainaut, C. R.: 1988, Opt. Eng. 27, 730 Google Scholar
[13] Beckers, J. M.: 1986, SPIE 628, p225 Google Scholar
[14] Beckers, J. M.: 1990, SPIE 1236, p379 Google Scholar
[15] Tallon-Bosc, I. and Tallon, M.: 1991, ESO Conf. on High Resolution Imaging by Interferometry II, Garching (Germany), Octobre 14–18 Google Scholar
[16] Faucherre, M., Merkle, F. and Vakili, F.: 1989, SPIE 1130, p138 Google Scholar
[17] Michelson, A. A. and Pease, F. G.: 1921, Astrophys. J. 53, 249.Google Scholar
[18] Mertz, L.: 1983, Appl. Opt. 22, 1530.Google Scholar
[19] Fried, D. L.: 1979, IAU Colloquium 50 on High Angular Resolution Stellar Interferometry, Sydney, N.S.W., Australia, (Davis, J. and Tango, W. J. Ed.), p4 Google Scholar
[20] Thompson, A. R., Moran, J. M. and Swenson, G. W. Jr.: 1986, “Interferometry and Synthesis in Radio Astronomy”, Wiley-Interscience Publ., New York Google Scholar