期刊
ASTROPHYSICAL JOURNAL
卷 812, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/812/2/176
关键词
cosmic background radiation; instrumentation: detectors; instrumentation: polarimeters; methods: laboratory: solid state; techniques: polarimetric
资金
- JPL Research and Technology Development Fund
- NASA [06-ARPA206-0040, 10-SAT10-0017]
- Gordon and Betty Moore Foundation at Caltech
- Canada Foundation for Innovation grant
- W. M. Keck Foundation
- US National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592, ANT-1110087]
- STFC [ST/K000926/1] Funding Source: UKRI
- Directorate For Geosciences
- Office of Polar Programs (OPP) [1145172] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [1125897] Funding Source: National Science Foundation
- Office of Polar Programs (OPP)
- Directorate For Geosciences [1145143] Funding Source: National Science Foundation
We have developed antenna-coupled transition-edge sensor bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including BICEP2, Keck Array, and the balloon borne SPIDER. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%-30% bandwidth at 95, 150, or 230 GHz. The integrated antenna arrays synthesize symmetric co-aligned beams with controlled side-lobe levels. Cross-polarized response on boresight is typically similar to 0.5%, consistent with cross-talk in our multiplexed readout system. End-to-end optical efficiencies in our cameras are routinely 35% or higher, with per detector sensitivities of NET similar to 300 mu K-CMB root s. Thanks to the scalability of this design, we have deployed 2560 detectors as 1280 matched pairs in Keck Array with a combined instantaneous sensitivity of similar to 9 mu K-CMB root s, as measured directly from CMB maps in the 2013 season. Similar arrays have recently flown in the SPIDER instrument, and development of this technology is ongoing.
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