Optimization and sensitivity of the Keck Array

Authors :: D. V. Wiebe
Peter A. R. Ade
C. L. Wongg
Abigail G. Vieregg
James J. Bock
C. L. Kuo
M. Lueker
Z. K. Staniszewski
A. D. Turner
John M Kovac
C. D. Dowell
C. D. Sheehy
R. V. Sudiwala
Justus A. Brevik
Kent D. Irwin
M. Amiri
L. Duband
G. P. Teply
R. W. Aikin
J. E. Tolan
Sunil Golwala
S. Fliescher
S. A. Kernasovskiy
M. Hasselfield
J. E. Ruhl
G. Hiltion
R. W. Ogburn
C. D. Reintsema
Roger O'Brient
G. Davis
Colin A. Bischoff
Calvin B. Netterfield
Jeffrey P. Filippini
P. R. Wilson
R. Schwarz
H. T. Nguyen
E. M. Leitch
J. A. Bonetti
Mark Halpern
B. Burger
C. Pryke
M. C. Runyan
S. J. Benton
V. V. Hristov
Holland, Wayne S.
Zmuidzinas, J.
Publication Year :: 2012
Publisher :: Society of Photo-Optical Instrumentation Engineers (SPIE), 2012.
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.<br />Comment: Presented at SPIE 2012 Astronomical Telescopes and Instrumentation Conference. Will be published in the proceedings

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