Optimization and sensitivity of the Keck Array

Creators: Kernasovskiy, S.; Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Dowell, C. D.; Filippini, J. P.; Golwala, S. R.; Hristov, V. V.; Lueker, M.; Nguyen, H. T.; O'Brient, R.; Runyan, M. C.; Staniszewski, Z.; Teply, G.

Others:: Holland, Wayne S.; Zmuidzinas, J.

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 µK_(CMB)√s in the 2012 configuration.

Additional Information

© 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). The Keck Array projects have been made possible through support from the National Science Foundation (grant Nos. ANT-1044978/ANT-1110087) and the Keck Foundation. Detector development has been made possible with the Gordon and Betty Moore foundation. We also acknowledge the Canada Foundation for Innovation and BC Knowledge Development Fund for support. We are grateful to Robert Schwarz for spending the winter in the South Pole for us in both 2011 and 2012, as well as to the South Pole logistics team. We also are grateful for the insight and collaboration from the entire Bicep2, SPIDER and Keck Array teams.

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