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Optimization and sensitivity of the Keck Array

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arxiv 1208.0857 v1 pith:VOBCGXME submitted 2012-08-03 astro-ph.IM astro-ph.CO

Optimization and sensitivity of the Keck Array

S. Kernasovskiy , P. A. R. Ade , R.W. Aikin , M. Amiri , S. Benton , C. Bischoff , J.J. Bock , J. A. Bonetti
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J. A. Brevik B. Burger G. Davis C.D. Dowell L. Duband J. P. Filippini S. Fliescher S.R. Golwala M. Halpern M. Hasselfield G. Hiltion V.V. Hristov K. Irwin J. M. Kovac C. L. Kuo E. Leitch M. Lueker C.B. Netterfield H. T. Nguyen R. O'Brient R. W. Ogburn IV C. L. Pryke C. Reintsema J.E. Ruhl M.C. Runyan R. Schwarz C. D. Sheehy Z. Staniszewski R. Sudiwala G. Teply J. E. Tolan A. D. Turner A. Vieregg D. V. Wiebe P. Wilson C. L. Wongg
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keywords arraykeckoptimizationsensitivityachievedantenna-coupledbackgroundbegan
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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, 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)*sqrt{s} in the 2012 configuration.

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