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The 2.5 m Telescope of the Sloan Digital Sky Survey

2006; Institute of Physics; Volume: 131; Issue: 4 Linguagem: Inglês

10.1086/500975

1538-3881

James E. Gunn, Walter A. Siegmund, Edward J. Mannery, Russell Owen, Charles L. H. Hull, R. French Leger, Larry Carey, G. R. Knapp, Donald G. York, William N. Boroski, S. Kent, Robert H. Lupton, Constance M. Rockosi, Michael L. Evans, Patrick Waddell, John E. Anderson, J. Annis, John C. Barentine, L. Bartoszek, Steven Bastian, S. B. Bracker, H. Brewington, C. Briegel, J. Brinkmann, Yorke J. Brown, Michael A. Carr, Paul C. Czarapata, C. Drennan, T. Dombeck, Glenn R. Federwitz, Bruce Gillespie, Carlos Gomez Gonzales, Sten Hansen, Michael Harvanek, J. J. E. Hayes, Wendell P. Jordan, E. Kinney, Mark A. Klaene, S. J. Kleinman, Richard G. Kron, Jurek Kresinski, Glenn Lee, Siriluk Limmongkol, C. Lindenmeyer, Daniel C. Long, Craig L. Loomis, P. McGehee, P. Mantsch, Eric H. Neilsen, Richard Neswold, Peter R. Newman, A. Nitta, J. Peoples, Jeffrey R. Pier, P. Prieto, Angela Prosapio, Claudio Rivetta, Donald P. Schneider, Stephanie A. Snedden, Shu-i Wang,

Astronomy and Astrophysical Research

We describe the design, construction, and performance of the Sloan Digital Sky Survey Telescope located at Apache Point Observatory. The telescope is a modified two-corrector Ritchey-Chretien design which has a 2.5-m, f/2.25 primary, a 1.08-m secondary, a Gascoigne astigmatism corrector, and one of a pair of interchangeable highly aspheric correctors near the focal focal plane, one for imaging and the other for spectroscopy. The final focal ratio is f/5. The telescope is instrumented by a wide-area, multiband CCD camera and a pair of fiber-fed double spectrographs. Novel features of the telescope include: (1) A 3 degree diameter (0.65 m) focal plane that has excellent image quality and small geometrical distortions over a wide wavelength range (3000 to 10,600 Angstroms) in the imaging mode, and good image quality combined with very small lateral and longitudinal color errors in the spectroscopic mode. The unusual requirement of very low distortion is set by the demands of time-delay-and-integrate (TDI) imaging; (2) Very high precision motion to support open loop TDI observations; and (3) A unique wind baffle/enclosure construction to maximize image quality and minimize construction costs. The telescope had first light in May 1998 and began regular survey operations in 2000.