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; 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. Hilton; 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. Wong

doi:10.1117/12.926934

27 September 2012 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, 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. Hilton, 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. Wong

Author Affiliations +

Proceedings Volume 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI; 84521B (2012) https://doi.org/10.1117/12.926934
Event: SPIE Astronomical Telescopes + Instrumentation, 2012, Amsterdam, Netherlands

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.

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S. Kernasovskiy, P. A. R. Ade, R. W. Aikin, M. Amiri, S. Benton, C. Bischoff, J. J. Bock, J. A. Bonetti, 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. Hilton, 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, and 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); https://doi.org/10.1117/12.926934

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