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A 4-meter McMath Telescope for the Infrared

Published online by Cambridge University Press:  03 August 2017

W. Livingston
W. Livingston*
Affiliation:
National Solar Observatory, P. 0. Box 26732, Tucson, AZ 85726, U.S.A.

Abstract

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Having no window and a filled aperture, i.e., no occlusion by secondary optics, the all-reflective McMath telescope is a proven IR facility. Beyond about 2 μm, it is diffraction limited, however. Engineering studies show that the McMath building could accommodate an increase to a 4-m aperture with a 6-m alt-azimuth feed, permitting sub-arcsec resolution to 12 μm. The use of cooled, solid aluminum mirrors would eliminate “mirror seeing”, which plagues non-vacuum solar telescopes.

Keywords

infrared: starsSun: generaltelescopes
Type
Part 7: Infrared Technology and the Future
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 589 - 594
Copyright
Copyright © Kluwer 1994 

References

Ayres, T. R. and Brault, J. W.: 1990, Astrophys. J. 363, 705.CrossRefGoogle Scholar
Ayres, T. R. and Testerman, L.: 1981, Astrophys. J. 245, 1124.CrossRefGoogle Scholar
Barr, L., Fox, J., Poczulp, G., and Roddier, C.: 1990, SPIE Proc. 1236, p. 492.Google Scholar
Boyd, R. W.: 1978, J. Opt. Soc. Am. 68, 877.Google Scholar
Carlsson, M., Rutten, R. J., and Shchukina, N. G.: 1992, Astron. Astrophys. 253, 567.Google Scholar
Deming, D., Hewagama, T., Jennings, D. E., and Wiedemann, G.: 1991, in November, L. (ed.), Solar Polarimetry, Proc. 11th Sacramento Peak Workshop, NSO, Sunspot, New Mexico, p. 341.Google Scholar
Deming, D., Hillman, J. J., Kostiuk, T., Mumma, M. J. and Zipoy, D. M.: 1984, Solar Phys. 94, 57.Google Scholar
Foukal, P., Little, R., Graves, J., Rabin, D., and Lynch, D.: 1990, Astrophys. J. 353, 712.Google Scholar
Hall, D. N. B.: 1970, Doctoral Dissertation, Harvard Univ., KPNO Contr. No. 556.Google Scholar
Harvey, J. and Hall, D. N. B.: 1975, Bull. Amer. Astron. Soc. 7, 459.Google Scholar
Harvey, J.: 1985, in Hagyard, M. J. (ed.) Measurements of Solar Vector Magnetic Fields, NASA Conf. Pub. 2374, NASA, Washington, D.C., 109.Google Scholar
Iye, M., Noguchi, T., Torii, Y., Mikami, Y., and Ando, H.: 1991, Pub. Astron. Soc. Pacific 103, 712.Google Scholar
Kopp, G. and Livingston, W.: 1991, private communication.Google Scholar
Livingston, W. and Barr, L.: 1992 in Giampapa, M. S. and Bookbinder, J. A. (eds.), Cool Stars, Stellar Systems, and the Sun, Seventh Cambridge Workshop, Astron. Soc. Pacific Conf. Ser. Vol. 26, San Francisco, p. 604.Google Scholar
Rabin, D., Jaksha, D., Plymate, C., Wagner, J., and Iwata, K.: 1991 in November, L. (ed.), Solar Polarimetry, Proc. 11th Sacramento Peak Workshop, NSO, Sunspot, New Mexico, p. 361.Google Scholar
Roddier, F. and Graves, J. E.: 1993, these proceedings.Google Scholar
Rozelot, J. P. and Leblanc, J.-M.: 1991, SPIE Proc., 1994, p. 481.Google Scholar
Solanki, S., Biémont, E., and Mürset, U.: 1990, Astron. Astrophys. Suppl. 83, 307.Google Scholar
Stenflo, J. O., Solanki, S. K., and Harvey, J. W.: 1987, Astrophys. J. 173, 167.Google Scholar
Turon, P. J. and Lena, P. J.: 1970, Solar Phys. 14, 112.Google Scholar
Wallace, L.: 1991, private communication.Google Scholar
Zirker, J. B.: 1985, Solar Phys. 102, 33–40.Google Scholar