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Infrared Speckle Interferometry: A Sensitive Technique for Physical Measurements of Unseen Companions to Nearby Stars

Published online by Cambridge University Press:  04 August 2017

D. W. McCarthy Jr.
D. W. McCarthy Jr.*
Affiliation:
Steward Observatory, The University of Arizona, Tucson, Arizona, USA

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Infrared speckle interferometry combines the full resolving power of large telescopes with high photometric sensitivity over the wavelength range 2.2 to 12 microns. Despite improved atmospheric seeing at these wavelengths, seeing fluctuations limit measurement precision. Astrometric companions have been detected with angular separations ≥0.1 arcsec and magnitude differences ≤3.7 mag. Results illustrate seeing limitations and show how the usual position angle ambiguity can be overcome. These measurements yield masses and absolute magnitudes for calibrating the lower main sequence. In some cases, orbital motion is detected. A method of “shift-and-add” enables detection of substellar (0.04 to 0.08 M⊙) companions. Future improvements involving detector arrays and seeing monitors are discussed.

Type
IV. Interferometry
Information
Symposium - International Astronomical Union , Volume 109: Astrometric Techniques , 1986 , pp. 309 - 319
Copyright
Copyright © Reidel 1986 

References

Bates, R. H. T., and Fright, W. R.: 1982, Monthly Notices Roy. Astron. Soc., 198, 1017.CrossRefGoogle Scholar
Dyck, H. M., and Howell, R. R.: 1983, Publ. Astron. Soc. Pacific, 95, 786.Google Scholar
Fried, D. L.: 1979, in Davis, J. and Tango, W. J. (ed.) High Angular Resolution Stellar Interferometry: Proc. of I.A.U. Colloq. No. 50, Sydney, p. 4-1.Google Scholar
Hogbom, J. A.: 1974, Astron. & Astrophys. Supl., 15, 417.Google Scholar
Howell, R. R.: 1980, , The University of Arizona.Google Scholar
Lippincott, S. L.: 1978, Space Sci. Rev., 22, 153.Google Scholar
Lippincott, S. L., Braun, D., and McCarthy, D. W.: 1983, Publ. Astron. Soc. Pacific, 95, 275.Google Scholar
Mariotti, J. M.: 1983, Optica Acta, 30, 831.CrossRefGoogle Scholar
McCarthy, D. W., Low, F. J., Kleinmann, S. G., and Arganbright, D. V.: 1982, Astrophys. J. (Letters), 257, L75.Google Scholar
McCarthy, D. W.: 1983, in The Nearby Stars and the Stellar Luminosity Function: Proc. of I.A.U. Colloq. No. 76, in press.Google Scholar
McCarthy, D. W.: 1984, Astron. J., in press.Google Scholar
Selby, M. J., Wade, R., and Magro, C.: 1979, Monthly Notices Roy. Astron. Soc., 187, 553.CrossRefGoogle Scholar
Sibille, F., Chelli, A., and Lena, P.: 1979, Astron. & Astrophys., 79 315.Google Scholar
Staller, R. F. A., and de Jong, T.: 1981, Astron. & Astrophys., 98, 140.Google Scholar
Stein, J. W., Kamper, K. W., and McCarthy, D. W.: 1984, in preparation.Google Scholar
Stevenson, D. J.: 1978, Proc. Astron. Soc. Australia, 3, 227.Google Scholar
Veeder, G. J.: 1975, Astron. J., 79, 1056.Google Scholar
Walker, J. G.: 1982, Appl. Opt., 21, 3132.Google Scholar