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Optimization And Sensitivity Of The Keck Array

S A Kernasovskiy,P A R Ade,R W Aikin,Mohammad Amin Amiri,S J Benton,C Bischoff,J J Bock,J A Bonetti,J A Brevik,B V Burger, G D Davis,C D Dowell,L Duband,J Filippini,S Fliescher,S R Golwala,M Halpern,M Hasselfield,G C Hilton,V V Hristov,K D Irwin,J Kovac,C L Kuo,E M Leitch,M Lueker,C B Netterfield,H T Nguyen,R Obrient,R W Ogburn,C Pryke,C D Reintsema,J E Ruhl,M C Runyan,Robert Schwarz,C D Sheehy,Z Staniszewski,R Sudiwala,G P Teply,J E Tolan,A D Turner,A G Vieregg,D V Wiebe,P Wilson,C L Wong

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY VI（2012）

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Abstract
The Keck Array (SPUD) began observing the cosmic microwave background's polarization in the winter of 2011 at the South Pole. The Keck Array follows the success of the predecessor experiments BICEP and BICEP2,1 using five on-axis refracting telescopes. These have a combined imaging array of 2500 antenna-coupled TES bolometers read with a SQUID-based time domain multiplexing system. We will discuss the detector noise and the optimization of the readout. The achieved sensitivity of the Keck Array is 11.5 mu K-CMB root s in the 2012 configuration.
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Key words
Cosmic Microwave Background, polarization, inflation, Keck Array, BICEP2, TES, detector noise
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