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Proceedings Paper

SWCam: the short wavelength camera for the CCAT Observatory
Author(s): Gordon J. Stacey; Stephen Parshley; Thomas Nikola; German Cortes-Medellin; Justin Schoenwald; Ganesh Rajagopalan; Michael D. Niemack; Tim Jenness; Patricio Gallardo; Brian Koopman; Charles D. Dowell; Peter K. Day; Matthew I. Hollister; Attila Kovacs; Henry G. LeDuc; Christopher M. McKenney; Ryan M. Monroe; Hiroshige Yoshida; Jonas Zmuidzinas; Loren J. Swenson; Simon J. Radford; Hien Trong Nguyen; Anthony K. Mroczkowski; Jason Glenn; Jordan Wheeler; Philip Maloney; Spencer Brugger; Joseph D. Adams; Frank Bertoldi; Reinhold Schaaf; Mark Halpern; Douglas Scott; Galen Marsden; Jack Sayers; Scott Chapman; Joaquin D. Vieira
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Paper Abstract

We describe the Short Wavelength Camera (SWCam) for the CCAT observatory including the primary science drivers, the coupling of the science drivers to the instrument requirements, the resulting implementation of the design, and its performance expectations at first light. CCAT is a 25 m submillimeter telescope planned to operate at 5600 meters, near the summit of Cerro Chajnantor in the Atacama Desert in northern Chile. CCAT is designed to give a total wave front error of 12.5 μm rms, so that combined with its high and exceptionally dry site, the facility will provide unsurpassed point source sensitivity deep into the short submillimeter bands to wavelengths as short as the 200 μm telluric window. The SWCam system consists of 7 sub-cameras that address 4 different telluric windows: 4 subcameras at 350 μm, 1 at 450 μm, 1 at 850 μm, and 1 at 2 mm wavelength. Each sub-camera has a 6’ diameter field of view, so that the total instantaneous field of view for SWCam is equivalent to a 16’ diameter circle. Each focal plane is populated with near unit filling factor arrays of Lumped Element Kinetic Inductance Detectors (LEKIDs) with pixels scaled to subtend an solid angle of (λ/D)2 on the sky. The total pixel count is 57,160. We expect background limited performance at each wavelength, and to be able to map < 35(°)2 of sky to 5 σ on the confusion noise at each wavelength per year with this first light instrument. Our primary science goal is to resolve the Cosmic Far-IR Background (CIRB) in our four colors so that we may explore the star and galaxy formation history of the Universe extending to within 500 million years of the Big Bang. CCAT's large and high-accuracy aperture, its fast slewing speed, use of instruments with large format arrays, and being located at a superb site enables mapping speeds of up to three orders of magnitude larger than contemporary or near future facilities and makes it uniquely sensitive, especially in the short submm bands.

Paper Details

Date Published: 19 August 2014
PDF: 16 pages
Proc. SPIE 9153, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 91530L (19 August 2014); doi: 10.1117/12.2057101
Show Author Affiliations
Gordon J. Stacey, Cornell Univ. (United States)
Stephen Parshley, Cornell Univ. (United States)
Thomas Nikola, Cornell Univ. (United States)
German Cortes-Medellin, Cornell Univ. (United States)
Justin Schoenwald, Cornell Univ. (United States)
Ganesh Rajagopalan, Cornell Univ. (United States)
Michael D. Niemack, Cornell Univ. (United States)
Tim Jenness, Cornell Univ. (United States)
Patricio Gallardo, Cornell Univ. (United States)
Brian Koopman, Cornell Univ. (United States)
Charles D. Dowell, California Institute of Technology (United States)
Peter K. Day, Jet Propulsion Lab. (United States)
Matthew I. Hollister, California Institute of Technology (United States)
Attila Kovacs, California Institute of Technology (United States)
Univ. of Minnesota (United States)
Henry G. LeDuc, Jet Propulsion Lab. (United States)
Christopher M. McKenney, California Institute of Technology (United States)
Ryan M. Monroe, Jet Propulsion Lab. (United States)
Hiroshige Yoshida, California Institute of Technology (United States)
Jonas Zmuidzinas, California Institute of Technology (United States)
Loren J. Swenson, California Institute of Technology (United States)
Simon J. Radford, California Institute of Technology (United States)
Hien Trong Nguyen, Jet Propulsion Lab. (United States)
Anthony K. Mroczkowski, California Institute of Technology (United States)
Jason Glenn, Univ. of Colorado at Boulder (United States)
Jordan Wheeler, Univ. of Colorado at Boulder (United States)
Philip Maloney, Univ. of Colorado at Boulder (United States)
Spencer Brugger, Univ. of Colorado at Boulder (United States)
Joseph D. Adams, SOFIA-Universities Space Research Association, NASA/Armstrong Flight Research Ctr. (United States)
Frank Bertoldi, Bonn Univ. (Germany)
Reinhold Schaaf, Bonn Univ. (Germany)
Mark Halpern, The Univ. of British Columbia (Canada)
Douglas Scott, The Univ. of British Columbia (Canada)
Galen Marsden, The Univ. of British Columbia (Canada)
Jack Sayers, California Institute of Technology (United States)
Scott Chapman, Dalhousie Univ. (Canada)
Joaquin D. Vieira, California Institute of Technology (United States)


Published in SPIE Proceedings Vol. 9153:
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII
Wayne S. Holland; Jonas Zmuidzinas, Editor(s)

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