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Characterization of a prototype SCUBA-2 1280-pixel submillimetre superconducting bolometer array

Zmuidzinas, Jonas, Woodcraft, Adam L., Hollister, Matthew I., Bintley, Dan, Ellis, Maureen A., Gao, Xiaofeng, Holland, Wayne S., MacIntosh, Michael J., Ade, Peter A. R., House, Julian Steven, Hunt, Cynthia L., Sudiwala, Rashmikant V., Duncan, William D., Hilton, Gene C., Irwin, Kent D., Reintsema, Carl D., Dunare, Camelia C., Parkes, William, Walton, Anthony J., Kycia, Jan B., Amiri, Mandana, Burger, Bryce, Halpern, Mark, Holland, Wayne S., Withington, Stafford and Duncan, William D. 2006. Characterization of a prototype SCUBA-2 1280-pixel submillimetre superconducting bolometer array. 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. Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III. Bellingham WA: The International Society for Optical Engineering, 62751F. 10.1117/12.671310

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Abstract

We present the results of characterization measurements on a 1280 pixel superconducting bolometer array designed for operation at wavelengths around 450 μm. The array is a prototype for the sub-arrays which will form the focal plane for the SCUBA-2 sub-mm camera, being built for the James Clerk Maxwell Telescope (JCMT) in Hawaii. With over 10 000 pixels in total, it will provide a huge improvement in both sensitivity and mapping speed over existing instruments. The array consists of molybdenum-copper bi-layer TES (transition edge sensor) pixels, bonded to a multiplexer. The detectors operate at a temperature of approximately 175 mK, and require a heat sink at a temperature of approximately 60 mK. In contrast to previous TES arrays, the multiplexing elements are located beneath each pixel (an "in-focal plane" configuration). We present the results of electrical and optical measurements, and show that the optical NEP (noise equivalent power) is less than 1.4 × 10-16 W Hz-0.5 and thus within the goal of 1.5 × 10-16 W Hz-0.5.

Item Type: Conference or Workshop Item (Paper)
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Uncontrolled Keywords: bolometers; superconductors; sensors; telescopes; cameras; copper; equipment and services; heatsinks; molybdenum; multiplexing
Publisher: The International Society for Optical Engineering
ISBN: 9780819463401
ISSN: 0277-786X
Related URLs:
Last Modified: 15 Dec 2017 10:58
URI: http://orca-mwe.cf.ac.uk/id/eprint/60366

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