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Title:
Instrumentation for the CCAT Telescope
Authors:
Stacey, G. J.; Golwala, S. R.; Bradford, C. M.; Dowell, C. D.; Cortes-Medellin, G.; Nikola, T.; Zmuidzinas, J.; Herter, T. L.; Radford, S. J.; Lloyd, J. P.; Blain, A. W.; Brown, R. L.; Campbell, D. B.; Giovanelli, R.; Goldsmith, P.; Harvey, P. M.; Henderson, C.; Langer, W. D.; Phillips, T. G.; Readhead, A. C. S.; Woody, D. P.
Affiliation:
AA(Cornell Univ. (USA)), AB(California Institute of Technology (USA)), AC(Jet Propulsion Lab. (USA)), AD(Jet Propulsion Lab. (USA)), AE(Cornell Univ. (USA)), AF(Cornell Univ. (USA)), AG(California Institute of Technology (USA)), AH(Cornell Univ. (USA)), AI(California Institute of Technology (USA)), AJ(Cornell Univ. (USA)), AK(California Institute of Technology (USA)), AL(Cornell Univ. (USA)), AM(Cornell Univ. (USA)), AN(Cornell Univ. (USA)), AO(Jet Propulsion Lab. (USA)), AP(Univ. of Texas, Austin (USA)), AQ(Cornell Univ. (USA)), AR(Jet Propulsion Lab. (USA)), AS(California Institute of Technology (USA)), AT(California Institute of Technology (USA)), AU(California Institute of TechnologyOwens Valley Radio Observatory (USA))
Publication:
Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III. Edited by Zmuidzinas, Jonas; Holland, Wayne S.; Withington, Stafford; Duncan, William D.. Proceedings of the SPIE, Volume 6275, pp. 62751G (2006). (SPIE Homepage)
Publication Date:
07/2006
Origin:
SPIE
DOI:
10.1117/12.672176
Bibliographic Code:
2006SPIE.6275E..47S

Abstract

We present a first cut instrument design package for the proposed 25 meter Cornell-Caltech Atacama Telescope (CCAT). The primary science for CCAT can be achieved through wide field photometric imaging in the short submillimeter through millimeter (200 μm to 2 mm) telluric windows. We present strawman designs for two cameras: a 32,000 pixel short submillimeter (200 to 650 μm) camera using transition edge sensed bare bolometer arrays that Nyquist samples (@ 350 μm) a 5'×5' field of view (FoV), and a 45,000 pixel long wavelength camera (850 μm to 2 mm) that uses slot dipole antennae coupled bolometer arrays with wavelength dependent sampling that covers up to a 20' square FoV. These are our first light instruments. We also anticipate "borrowed" instruments such as direct detection and heterodyne detection spectrometers will be available at, or nearly at first light.
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