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TES imaging array technology for CℓOVER

Zmuidzinas, Jonas, Audley, Michael D., Barker, Robert W., Crane, Michael, Dace, Roger, Glowacka, Dorota, Goldie, David J., Lasenby, Anthony N., Stevenson, Howard M., Tsaneva, Vassilka, Withington, Stafford, Grimes, Paul, Johnson, Bradley, Yassin, Ghassan, Piccirillo, Lucio, Pisano, Giampaolo, Duncan, William D., Hilton, Gene C., Irwin, Kent D., Reintsema, Carl D., Halpern, Mark, Holland, Wayne S., Withington, Stafford and Duncan, William D. 2006. TES imaging array technology for CℓOVER. Presented at: Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III, Orlando, FL, USA, 29-31 May 2006. Published in: Zmuidzinas, Jonas, Holland, Wayne S., Withington, Stafford and Duncan, William D. eds. Proceedings SPIE 6275, Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III. The International Society for Optical Engineering, p. 627524. 10.1117/12.670792

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Abstract

CℓOVER 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. CℓOVER 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 CℓOVER 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 CℓOVER detectors, detector blocks, and readout, and give an update on the detector development.

Item Type: Conference or Workshop Item (Paper)
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Publisher: The International Society for Optical Engineering
ISSN: 0277-786X
Related URLs:
Last Modified: 04 Jun 2017 06:31
URI: http://orca-mwe.cf.ac.uk/id/eprint/61443

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