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. Hiltion, V.V. Hristov, K. Irwin
TL;DR
The paper discusses the optimization, sensitivity, and detector noise characteristics of the Keck Array, a telescope array designed to observe the cosmic microwave background polarization from the South Pole, highlighting its improved sensitivity and technical setup.
Contribution
It presents the detector noise analysis and readout optimization of the Keck Array, enhancing its sensitivity for CMB polarization measurements.
Findings
Achieved sensitivity of 11.5 μK√s in 2012 configuration.
Optimized readout system for TES bolometers.
Analyzed detector noise performance.
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, 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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