27 September 2012 Optimization and sensitivity of the Keck array
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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 μKCMB√s in the 2012 configuration.
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S. Kernasovskiy, S. Kernasovskiy, P. A. R. Ade, P. A. R. Ade, R. W. Aikin, R. W. Aikin, M. Amiri, M. Amiri, S. Benton, S. Benton, C. Bischoff, C. Bischoff, J. J. Bock, J. J. Bock, J. A. Bonetti, J. A. Bonetti, J. A. Brevik, J. A. Brevik, B. Burger, B. Burger, G. Davis, G. Davis, C. D. Dowell, C. D. Dowell, L. Duband, L. Duband, J. P. Filippini, J. P. Filippini, S. Fliescher, S. Fliescher, S. R. Golwala, S. R. Golwala, M. Halpern, M. Halpern, M. Hasselfield, M. Hasselfield, G. Hilton, G. Hilton, V. V. Hristov, V. V. Hristov, K. Irwin, K. Irwin, J. M. Kovac, J. M. Kovac, C. L. Kuo, C. L. Kuo, E. Leitch, E. Leitch, M. Lueker, M. Lueker, C. B. Netterfield, C. B. Netterfield, H. T. Nguyen, H. T. Nguyen, R. O'Brient, R. O'Brient, R. W. Ogburn, R. W. Ogburn, C. L. Pryke, C. L. Pryke, C. Reintsema, C. Reintsema, J. E. Ruhl, J. E. Ruhl, M. C. Runyan, M. C. Runyan, R. Schwarz, R. Schwarz, C. D. Sheehy, C. D. Sheehy, Z. Staniszewski, Z. Staniszewski, R. Sudiwala, R. Sudiwala, G. Teply, G. Teply, J. E. Tolan, J. E. Tolan, A. D. Turner, A. D. Turner, A. Vieregg, A. Vieregg, D. V. Wiebe, D. V. Wiebe, P. Wilson, P. Wilson, C. L. Wong, C. L. Wong, } "Optimization and sensitivity of the Keck array", Proc. SPIE 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 84521B (27 September 2012); doi: 10.1117/12.926934; https://doi.org/10.1117/12.926934
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