CCAT optics

S. Padin; M. Hollister; S. Radford; J. Sayers; D. Woody; J. Zmuidzinas; G. Cortes-Medellin; T. Sebring; G. Stacey

doi:10.1117/12.856489

5 August 2010 CCAT optics

S. Padin, M. Hollister, S. Radford, J. Sayers, D. Woody, J. Zmuidzinas, G. Cortes-Medellin, T. Sebring, G. Stacey

Proceedings Volume 7733, Ground-based and Airborne Telescopes III; 77334Y (2010) https://doi.org/10.1117/12.856489
Event: SPIE Astronomical Telescopes + Instrumentation, 2010, San Diego, California, United States

Abstract

CCAT will be a 25 m diameter, submillimeter-wave telescope. It will be located on Cerro Chajnantor in the Atacama Desert, near ALMA. CCAT will be an on-axis, Ritchey-Chrétien design with an active primary to compensate gravitational deformations. The primary mirror will have 162 segments, each with ~0.5 × 0.5 m reflecting tiles on a ~2×2 m, insulated, carbon-fiber-reinforced-plastic subframe. CCAT will be equipped with wide-field, multi-color cameras and multi-object spectrometers at its Nasmyth foci. These instruments will cover all the atmospheric windows in the λ = 0.2 to 2 mm range. The field of view at the Nasmyth foci will be 1°, so CCAT will be able to support cameras with a few ×10⁴ detectors (spaced 2 beamwidths) at λ = 1 mm to a few ×10⁶ detectors (spaced half a beamwidth) at λ = 350 μm. Single instruments of this size are probably impractical, so we will break the field into smaller pieces, with a separate sub-field camera for each piece. The cameras will require some relay optics to couple the fairly slow beam from the telescope to the detectors. A reflective relay for 1° field of view is too large to be practical, so we plan to use a compact, cold, refractive relay in each sub-field camera.

Citation Download Citation

S. Padin, M. Hollister, S. Radford, J. Sayers, D. Woody, J. Zmuidzinas, G. Cortes-Medellin, T. Sebring, and G. Stacey "CCAT optics", Proc. SPIE 7733, Ground-based and Airborne Telescopes III, 77334Y (5 August 2010); https://doi.org/10.1117/12.856489

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