TY - GEN
T1 - SWCam
T2 - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII
AU - Stacey, Gordon J.
AU - Parshley, Stephen
AU - Nikola, Thomas
AU - Cortes-Medellin, German
AU - Schoenwald, Justin
AU - Rajagopalan, Ganesh
AU - Niemack, Michael D.
AU - Jenness, Tim
AU - Gallardo, Patricio
AU - Koopman, Brian
AU - Dowell, Charles D.
AU - Day, Peter K.
AU - Hollister, Matthew I.
AU - Kovacs, Attila
AU - Leduc, Henry G.
AU - McKenney, Christopher M.
AU - Monroe, Ryan M.
AU - Yoshida, Hiroshige
AU - Zmuidzinas, Jonas
AU - Swenson, Loren J.
AU - Radford, Simon J.
AU - Nguyen, Hien Trong
AU - Mroczkowski, Anthony K.
AU - Glenn, Jason
AU - Wheeler, Jordan
AU - Maloney, Philip
AU - Brugger, Spencer
AU - Adams, Joseph D.
AU - Bertoldi, Frank
AU - Schaaf, Reinhold
AU - Halpern, Mark
AU - Scott, Douglas
AU - Marsden, Galen
AU - Sayers, Jack
AU - Chapman, Scott
AU - Vieira, Joaquin D.
N1 - Publisher Copyright:
© 2014 SPIE.
PY - 2014
Y1 - 2014
N2 - 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 Î1/4m 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 Î1/4m telluric window. The SWCam system consists of 7 sub-cameras that address 4 different telluric windows: 4 subcameras at 350 Î1/4m, 1 at 450 Î1/4m, 1 at 850 Î1/4m, and 1 at 2 mm wavelength. Each sub-camera has a 60% 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 (Î"/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 Ï 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.
AB - 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 Î1/4m 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 Î1/4m telluric window. The SWCam system consists of 7 sub-cameras that address 4 different telluric windows: 4 subcameras at 350 Î1/4m, 1 at 450 Î1/4m, 1 at 850 Î1/4m, and 1 at 2 mm wavelength. Each sub-camera has a 60% 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 (Î"/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 Ï 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.
KW - CCAT telescope
KW - LEKID detectors
KW - high redshift universe
KW - submillimeter cameras
KW - submillimeter galaxies
UR - http://www.scopus.com/inward/record.url?scp=84922837679&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84922837679&partnerID=8YFLogxK
U2 - 10.1117/12.2057101
DO - 10.1117/12.2057101
M3 - Conference contribution
AN - SCOPUS:84922837679
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII
A2 - Zmuidzinas, Jonas
A2 - Holland, Wayne S.
PB - SPIE
Y2 - 24 June 2014 through 27 June 2014
ER -