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Proceedings Paper

TES imaging array technology for COVER
Author(s): Michael D. Audley; Robert W. Barker; Michael Crane; Roger Dace; Dorota Glowacka; David J. Goldie; Anthony N. Lasenby; Howard M. Stevenson; Vassilka Tsaneva; Stafford Withington; Paul Grimes; Bradley Johnson; Ghassan Yassin; Lucio Piccirillo; Giampaolo Pisano; William D. Duncan; Gene C. Hilton; Kent D. Irwin; Carl D. Reintsema; Mark Halpern
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Paper Abstract

COVER is an experiment which aims to detect the signature of gravitational waves from inflation by measuring the B-mode polarization of the cosmic microwave background. COVER consists of three telescopes operating at 97, 150, and 220 GHz. The 97-GHz telescope has 160 horns in its focal plane while the 150 and 220-GHz telescopes have 256 horns each. The horns are arranged in a hexagonal array and feed a polarimeter which uses finline-coupled TES bolometers as detectors. To detect the two polarizations the 97-GHz telescope has 320 detectors while the 150 and 220-GHz telescopes have 512 detectors each. To achieve the required NEPs the detectors are cooled to 100 mK for the 97 and 150-GHz polarimeters and 230 mK for the 220-GHz polarimeter. Each detector is fabricated as a single chip to guarantee fully functioning focal planes. The detectors are contained in linear modules made of copper which form split-block waveguides. The detector modules contain 16 or 20 detectors each for compatibility with the hexagonal arrays of horns in the telescopes' focal planes. Each detector module contains a time-division SQUID multiplexer to read out the detectors. Further amplification of the multiplexed signals is provided by SQUID series arrays. The first prototype detectors for COVER operate with a bath temperature of 230 mK and are used to validate the detector design as well as the polarimeter technology. We describe the design of the COVER detectors, detector blocks, and readout, and give an update on the detector development.

Paper Details

Date Published: 16 June 2006
PDF: 9 pages
Proc. SPIE 6275, Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III, 627524 (16 June 2006); doi: 10.1117/12.670792
Show Author Affiliations
Michael D. Audley, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Robert W. Barker, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Michael Crane, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Roger Dace, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Dorota Glowacka, Cavendish Lab., Univ. of Cambridge (United Kingdom)
David J. Goldie, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Anthony N. Lasenby, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Howard M. Stevenson, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Vassilka Tsaneva, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Stafford Withington, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Paul Grimes, Univ. of Oxford (United Kingdom)
Bradley Johnson, Univ. of Oxford (United Kingdom)
Ghassan Yassin, Univ. of Oxford (United Kingdom)
Lucio Piccirillo, Cardiff Univ. (United Kingdom)
Giampaolo Pisano, Cardiff Univ. (United Kingdom)
William D. Duncan, National Institute of Standards and Technology (United States)
Gene C. Hilton, National Institute of Standards and Technology (United States)
Kent D. Irwin, National Institute of Standards and Technology (United States)
Carl D. Reintsema, National Institute of Standards and Technology (United States)
Mark Halpern, Univ. of British Columbia (Canada)


Published in SPIE Proceedings Vol. 6275:
Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III
Jonas Zmuidzinas; Wayne S. Holland; Stafford Withington; William D. Duncan, Editor(s)

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