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.
Cite
@article{arxiv.1208.0857,
title = {Optimization and sensitivity of the Keck Array},
author = {S. Kernasovskiy and P. A. R. Ade and R. W. Aikin and M. Amiri and S. Benton and C. Bischoff and J. J. Bock and J. A. Bonetti and J. A. Brevik and B. Burger and G. Davis and C. D. Dowell and L. Duband and J. P. Filippini and S. Fliescher and S. R. Golwala and M. Halpern and M. Hasselfield and G. Hiltion and V. V. Hristov and K. Irwin and J. M. Kovac and C. L. Kuo and E. Leitch and M. Lueker and C. B. Netterfield and H. T. Nguyen and R. O'Brient and R. W. Ogburn and C. L. Pryke and C. Reintsema and J. E. Ruhl and M. C. Runyan and R. Schwarz and C. D. Sheehy and Z. Staniszewski and R. Sudiwala and G. Teply and J. E. Tolan and A. D. Turner and A. Vieregg and D. V. Wiebe and P. Wilson and C. L. Wongg},
journal= {arXiv preprint arXiv:1208.0857},
year = {2015}
}
Comments
Presented at SPIE 2012 Astronomical Telescopes and Instrumentation Conference. Will be published in the proceedings