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Optimization and sensitivity of the Keck Array

Kernasovskiy, S. and Aikin, R. W. and Bock, J. J. and Brevik, J. A. and Dowell, C. D. and Filippini, J. P. and Golwala, S. R. and Hristov, V. V. and Lueker, M. and Nguyen, H. T. and O'Brient, R. and Runyan, M. C. and Staniszewski, Z. and Teply, G. (2012) Optimization and sensitivity of the Keck Array. In: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI. Proceedings of SPIE. No.8452. Society of Photo-Optical Instrumentation Engineers (SPIE) , Bellingham, WA, Art. No. 84521B. ISBN 978-0-8194-9153-4. https://resolver.caltech.edu/CaltechAUTHORS:20161025-122633225

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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 µK_(CMB)√s in the 2012 configuration.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1117/12.926934DOIArticle
https://arxiv.org/abs/1208.0857arXivDiscussion Paper
ORCID:
AuthorORCID
Bock, J. J.0000-0002-5710-5212
Filippini, J. P.0000-0001-8217-6832
Golwala, S. R.0000-0002-1098-7174
Additional Information:© 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). The Keck Array projects have been made possible through support from the National Science Foundation (grant Nos. ANT-1044978/ANT-1110087) and the Keck Foundation. Detector development has been made possible with the Gordon and Betty Moore foundation. We also acknowledge the Canada Foundation for Innovation and BC Knowledge Development Fund for support. We are grateful to Robert Schwarz for spending the winter in the South Pole for us in both 2011 and 2012, as well as to the South Pole logistics team. We also are grateful for the insight and collaboration from the entire Bicep2, SPIDER and Keck Array teams.
Funders:
Funding AgencyGrant Number
NSFANT-1044978
NSFANT-1110087
W. M. Keck FoundationUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
British Columbia Knowledge Development FundUNSPECIFIED
Subject Keywords:Cosmic Microwave Background, polarization, inflation, Keck Array, Bicep2, TES, detector noise
Series Name:Proceedings of SPIE
Issue or Number:8452
Record Number:CaltechAUTHORS:20161025-122633225
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20161025-122633225
Official Citation: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 ; 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 (September 27, 2012); doi:10.1117/12.926934; http://dx.doi.org/10.1117/12.926934
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:71454
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:25 Oct 2016 20:22
Last Modified:10 Dec 2019 21:42

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