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; J. M. Kovac; C. L. Kuo; E. Leitch; M. Lueker; C. B. Netterfield; H. T. Nguyen; R. O'Brient; R. W. Ogburn IV; 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; C. L. Wong

doi:10.1117/12.926934

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. HristovK. Irwin, J. M. Kovac, C. L. Kuo, E. Leitch, M. Lueker, C. B. Netterfield, H. T. Nguyen, R. O'Brient, R. W. Ogburn IV, 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, C. L. Wong

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

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.

Original language	English (US)
Title of host publication	Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI
DOIs	https://doi.org/10.1117/12.926934
State	Published - 2012
Externally published	Yes
Event	Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI - Amsterdam, Netherlands Duration: Jul 3 2012 → Jul 6 2012

Publication series

Name	Proceedings of SPIE - The International Society for Optical Engineering
Volume	8452
ISSN (Print)	0277-786X

Other

Other	Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI
Country/Territory	Netherlands
City	Amsterdam
Period	7/3/12 → 7/6/12

Keywords

Bicep2
Cosmic microwave background
Detector noise
Inflation
Keck array
Polarization
TES

ASJC Scopus subject areas

Electronic, Optical and Magnetic Materials
Condensed Matter Physics
Computer Science Applications
Applied Mathematics
Electrical and Electronic Engineering

Online availability

10.1117/12.926934

Library availability

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Cite this

Kernasovskiy, S., Ade, P. A. R., Aikin, R. W., Amiri, M., Benton, S., Bischoff, C., Bock, J. J., Bonetti, J. A., Brevik, J. A., Burger, B., Davis, G., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S., Golwala, S. R., Halpern, M., Hasselfield, M., Hiltion, G., ... Wong, C. L. (2012). Optimization and sensitivity of the Keck Array. In Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI Article 84521B (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 8452). https://doi.org/10.1117/12.926934

Optimization and sensitivity of the Keck Array. / Kernasovskiy, S.; Ade, P. A.R.; Aikin, R. W. et al.
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI. 2012. 84521B (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 8452).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Kernasovskiy, S, Ade, PAR, Aikin, RW, Amiri, M, Benton, S, Bischoff, C, Bock, JJ, Bonetti, JA, Brevik, JA, Burger, B, Davis, G, Dowell, CD, Duband, L, Filippini, JP, Fliescher, S, Golwala, SR, Halpern, M, Hasselfield, M, Hiltion, G, Hristov, VV, Irwin, K, Kovac, JM, Kuo, CL, Leitch, E, Lueker, M, Netterfield, CB, Nguyen, HT, O'Brient, R, Ogburn IV, RW, Pryke, CL, Reintsema, C, Ruhl, JE, Runyan, MC, Schwarz, R, Sheehy, CD, Staniszewski, Z, Sudiwala, R, Teply, G, Tolan, JE, Turner, AD, Vieregg, A, Wiebe, DV, Wilson, P & Wong, CL 2012, Optimization and sensitivity of the Keck Array. in Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI., 84521B, Proceedings of SPIE - The International Society for Optical Engineering, vol. 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, Amsterdam, Netherlands, 7/3/12. https://doi.org/10.1117/12.926934

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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 μKCMB√s in the 2012 configuration.",

keywords = "Bicep2, Cosmic microwave background, Detector noise, Inflation, Keck array, Polarization, TES",

author = "S. Kernasovskiy and Ade, {P. A.R.} and Aikin, {R. W.} and M. Amiri and S. Benton and C. Bischoff and Bock, {J. J.} and Bonetti, {J. A.} and Brevik, {J. A.} and B. Burger and G. Davis and Dowell, {C. D.} and L. Duband and Filippini, {J. P.} and S. Fliescher and Golwala, {S. R.} and M. Halpern and M. Hasselfield and G. Hiltion and Hristov, {V. V.} and K. Irwin and Kovac, {J. M.} and Kuo, {C. L.} and E. Leitch and M. Lueker and Netterfield, {C. B.} and Nguyen, {H. T.} and R. O'Brient and {Ogburn IV}, {R. W.} and Pryke, {C. L.} and C. Reintsema and Ruhl, {J. E.} and Runyan, {M. C.} and R. Schwarz and Sheehy, {C. D.} and Z. Staniszewski and R. Sudiwala and G. Teply and Tolan, {J. E.} and Turner, {A. D.} and A. Vieregg and Wiebe, {D. V.} and P. Wilson and Wong, {C. L.}",

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T1 - Optimization and sensitivity of the Keck Array

AU - Kernasovskiy, S.

AU - Ade, P. A.R.

AU - Aikin, R. W.

AU - Amiri, M.

AU - Benton, S.

AU - Bischoff, C.

AU - Bock, J. J.

AU - Bonetti, J. A.

AU - Brevik, J. A.

AU - Burger, B.

AU - Davis, G.

AU - Dowell, C. D.

AU - Duband, L.

AU - Filippini, J. P.

AU - Fliescher, S.

AU - Golwala, S. R.

AU - Halpern, M.

AU - Hasselfield, M.

AU - Hiltion, G.

AU - Hristov, V. V.

AU - Irwin, K.

AU - Kovac, J. M.

AU - Kuo, C. L.

AU - Leitch, E.

AU - Lueker, M.

AU - Netterfield, C. B.

AU - Nguyen, H. T.

AU - O'Brient, R.

AU - Ogburn IV, R. W.

AU - Pryke, C. L.

AU - Reintsema, C.

AU - Ruhl, J. E.

AU - Runyan, M. C.

AU - Schwarz, R.

AU - Sheehy, C. D.

AU - Staniszewski, Z.

AU - Sudiwala, R.

AU - Teply, G.

AU - Tolan, J. E.

AU - Turner, A. D.

AU - Vieregg, A.

AU - Wiebe, D. V.

AU - Wilson, P.

AU - Wong, C. L.

PY - 2012

Y1 - 2012

N2 - 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 μKCMB√s in the 2012 configuration.

AB - 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 μKCMB√s in the 2012 configuration.

KW - Bicep2

KW - Cosmic microwave background

KW - Detector noise

KW - Inflation

KW - Keck array

KW - Polarization

KW - TES

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U2 - 10.1117/12.926934

DO - 10.1117/12.926934

M3 - Conference contribution

AN - SCOPUS:84872094708

SN - 9780819491534

T3 - Proceedings of SPIE - The International Society for Optical Engineering

BT - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI

T2 - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI

Y2 - 3 July 2012 through 6 July 2012

ER -

Optimization and sensitivity of the Keck Array

Abstract

Publication series

Other

Keywords

ASJC Scopus subject areas

Online availability

Library availability

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