28 September 2004 ALMA front-end optics
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Abstract
The ALMA telescope will be an interferometer of 64 antennas, which will be situated in the Atacama desert in Chile. Each antenna will have receivers that cover the frequencies 30 GHz to 970 GHZ. This frequency range is divided into 10 frequency bands. All of these receiver bands are fitted on a cartridge and cooled, with bands 1 and 2 at 15K and the other 8 are SIS receivers at a temperature of 4K. Each band has a dual polarization receiver. The optics has been designed so that the maximum of the optics is cooled to minimize the noise temperature increase to the receivers. The design of the optics will be shown for each frequency bands. Test results with the method of testing on a near field amplitude and phase measurement system will be given for the first 4 frequency bands to be used, which are bands 3 (84-116 GHz), 6 (211-275GHz), 7 (275-375 GHz and 9 (600-702 GHz). These measurements will be compared with physical optics calculations.
© (2004) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Matthew C. Carter, Matthew C. Carter, Andrey Baryshev, Andrey Baryshev, Mark Harman, Mark Harman, Bernard Lazareff, Bernard Lazareff, James Lamb, James Lamb, Santiago Navarro, Santiago Navarro, Dave John, Dave John, A.-L. Fontana, A.-L. Fontana, Geoffrey Ediss, Geoffrey Ediss, Choy Yoong Tham, Choy Yoong Tham, Stafford Withington, Stafford Withington, Felix Tercero, Felix Tercero, Renzo Nesti, Renzo Nesti, Gie-Han Tan, Gie-Han Tan, Yutaro Sekimoto, Yutaro Sekimoto, Mayumi Matsunaga, Mayumi Matsunaga, Higawo Ogawa, Higawo Ogawa, Stephane Claude, Stephane Claude, } "ALMA front-end optics", Proc. SPIE 5489, Ground-based Telescopes, (28 September 2004); doi: 10.1117/12.552538; https://doi.org/10.1117/12.552538
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