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Keck array and BICEP3: spectral characterization of 5000+ detectors

Karkare, K. S. and Aikin, R. W. and Bock, J. J. and Brevik, J. A. and Crill, B. P. and Filippini, J. P. and Golwala, S. R. and Hildebrandt, S. R. and Hristov, V. V. and Hui, H. and Kefeli, S. and Lueker, M. and Mason, P. and Staniszewski, Z. K. and Teply, G. P. and Weber, A. (2014) Keck array and BICEP3: spectral characterization of 5000+ detectors. In: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII. Proceedings of SPIE. No.9153. Society of Photo-Optical Instrumentation Engineers (SPIE) , Bellingham, WA, Art. No. 91533B. ISBN 978-0-8194-9621-8.

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The inflationary paradigm of the early universe predicts a stochastic background of gravitational waves which would generate a B-mode polarization pattern in the cosmic microwave background (CMB) at degree angular scales. Precise measurement of B-modes is one of the most compelling observational goals in modern cosmology. Since 2011, the Keck Array has deployed over 2500 transition edge sensor (TES) bolometer detectors at 100 and 150 GHz to the South Pole in pursuit of degree-scale B-modes, and Bicep3 will follow in 2015 with 2500 more at 100 GHz. Characterizing the spectral response of these detectors is important for controlling systematic effects that could lead to leakage from the temperature to polarization signal, and for understanding potential coupling to atmospheric and astrophysical emission lines. We present complete spectral characterization of the Keck Array detectors, made with a Martin-Puplett Fourier Transform Spectrometer at the South Pole, and preliminary spectra of Bicep3 detectors taken in lab. We show band centers and effective bandwidths for both Keck Array bands, and use models of the atmosphere at the South Pole to cross check our absolute calibration. Our procedure for obtaining interferograms in the field with automated 4-axis coupling to the focal plane represents an important step towards efficient and complete spectral characterization of next-generation instruments more than 10000 detectors.

Item Type:Book Section
Related URLs:
URLURL TypeDescription
Karkare, K. S.0000-0002-5215-6993
Bock, J. J.0000-0002-5710-5212
Crill, B. P.0000-0002-4650-8518
Filippini, J. P.0000-0001-8217-6832
Golwala, S. R.0000-0002-1098-7174
Mason, P.0000-0002-7963-7420
Additional Information:© 2014 Society of Photo-Optical Instrumentation Engineers (SPIE). The Keck Array and Bicep3 projects have been made possible through support from the National Science Foundation (grant Nos. 0742818, 0742592, 1044978, 1110087, 1145172, 1313158, 1313010, 1313062, 1313287, 1056465, and 0960243), the W. M. Keck Foundation, the Canada Foundation for Innovation, and the British Columbia Development Fund. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA ARPA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. The computations in these proceedings were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Tireless administrative support was provided by Irene Coyle, Kathy Deniston, Donna Hernandez, and Dana Volponi. We are grateful to Robert Schwarz as our 2011–2014 Keck Array winterover. We thank the staff of the US Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank our Bicep1, Bicep2, and Spider colleagues for useful discussions and shared expertise.
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
British Columbia Development FundUNSPECIFIED
JPL Research and Technology Development FundUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
Harvard UniversityUNSPECIFIED
Subject Keywords:Inflation, Gravitational waves, Cosmic microwave background, Polarization, BICEP, Keck Array
Series Name:Proceedings of SPIE
Issue or Number:9153
Record Number:CaltechAUTHORS:20150615-105627198
Persistent URL:
Official Citation:K. S. Karkare ; P. A. R. Ade ; Z. Ahmed ; R. W. Aikin ; K. D. Alexander ; M. Amiri ; D. Barkats ; S. J. Benton ; C. A. Bischoff ; J. J. Bock ; J. A. Bonetti ; J. A. Brevik ; I. Buder ; E. W. Bullock ; B. Burger ; J. Connors ; B. P. Crill ; G. Davis ; C. D. Dowell ; L. Duband ; J. P. Filippini ; S. T. Fliescher ; S. R. Golwala ; M. S. Gordon ; J. A. Grayson ; M. Halpern ; M. Hasselfield ; S. R. Hildebrandt ; G. C. Hilton ; V. V. Hristov ; H. Hui ; K. D. Irwin ; J. H. Kang ; E. Karpel ; S. Kefeli ; S. A. Kernasovskiy ; J. M. Kovac ; C. L. Kuo ; E. M. Leitch ; M. Lueker ; P. Mason ; K. G. Megerian ; C. B. Netterfield ; H. T. Nguyen ; R. O'Brient ; R. W. Ogburn ; C. L. Pryke ; C. D. Reintsema ; S. Richter ; R. Schwarz ; C. D. Sheehy ; Z. K. Staniszewski ; R. V. Sudiwala ; G. P. Teply ; K. L. Thompson ; J. E. Tolan ; A. D. Turner ; A. Vieregg ; A. Weber ; C. L. Wong ; W. L. K. Wu ; K. W. Yoon; Keck array and BICEP3: spectral characterization of 5000+ detectors. Proc. SPIE 9153, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 91533B (August 19, 2014); doi:10.1117/12.2056779
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:58245
Deposited By: Tony Diaz
Deposited On:15 Jun 2015 18:11
Last Modified:09 Mar 2020 13:18

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