Optical Characterization of the SPT-3G Camera

Z. Pan; P. A.R. Ade; Z. Ahmed; A. J. Anderson; J. E. Austermann; J. S. Avva; R. Basu Thakur; A. N. Bender; B. A. Benson; J. E. Carlstrom; F. W. Carter; T. Cecil; C. L. Chang; J. F. Cliche; A. Cukierman; E. V. Denison; T. de Haan; J. Ding; M. A. Dobbs; D. Dutcher; W. Everett; A. Foster; R. N. Gannon; A. Gilbert; J. C. Groh; N. W. Halverson; A. H. Harke-Hosemann; N. L. Harrington; J. W. Henning; G. C. Hilton; W. L. Holzapfel; N. Huang; K. D. Irwin; O. B. Jeong; M. Jonas; T. Khaire; A. M. Kofman; M. Korman; D. Kubik; S. Kuhlmann; C. L. Kuo; A. T. Lee; A. E. Lowitz; S. S. Meyer; D. Michalik; J. Montgomery; A. Nadolski; T. Natoli; H. Nguyen; G. I. Noble; V. Novosad; S. Padin; J. Pearson; C. M. Posada; A. Rahlin; J. E. Ruhl; L. J. Saunders; J. T. Sayre; I. Shirley; E. Shirokoff; G. Smecher; J. A. Sobrin; A. A. Stark; K. T. Story; A. Suzuki; Q. Y. Tang; K. L. Thompson; C. Tucker; L. R. Vale; K. Vanderlinde; J. D. Vieira; G. Wang; N. Whitehorn; V. Yefremenko; K. W. Yoon; M. R. Young

doi:10.1007/s10909-018-1935-y

Optical Characterization of the SPT-3G Camera

Z. Pan, P. A.R. Ade, Z. Ahmed, A. J. Anderson, J. E. Austermann, J. S. Avva, R. Basu Thakur, A. N. Bender, B. A. Benson, J. E. Carlstrom, F. W. Carter, T. Cecil, C. L. Chang, J. F. Cliche, A. Cukierman, E. V. Denison, T. de Haan, J. Ding, M. A. Dobbs, D. DutcherW. Everett, A. Foster, R. N. Gannon, A. Gilbert, J. C. Groh, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, W. L. Holzapfel, N. Huang, K. D. Irwin, O. B. Jeong, M. Jonas, T. Khaire, A. M. Kofman, M. Korman, D. Kubik, S. Kuhlmann, C. L. Kuo, A. T. Lee, A. E. Lowitz, S. S. Meyer, D. Michalik, J. Montgomery, A. Nadolski, T. Natoli, H. Nguyen, G. I. Noble, V. Novosad, S. Padin, J. Pearson, C. M. Posada, A. Rahlin, J. E. Ruhl, L. J. Saunders, J. T. Sayre, I. Shirley, E. Shirokoff, G. Smecher, J. A. Sobrin, A. A. Stark, K. T. Story, A. Suzuki, Q. Y. Tang, K. L. Thompson, C. Tucker, L. R. Vale, K. Vanderlinde, J. D. Vieira, G. Wang, N. Whitehorn, V. Yefremenko, K. W. Yoon, M. R. Young

Research output: Contribution to journal › Article › peer-review

Abstract

The third-generation South Pole Telescope camera is designed to measure the cosmic microwave background across three frequency bands (centered at 95, 150 and 220 GHz) with ∼ 16,000 transition-edge sensor (TES) bolometers. Each multichroic array element on a detector wafer has a broadband sinuous antenna that couples power to six TESs, one for each of the three observing bands and both polarizations, via lumped element filters. Ten detector wafers populate the detector array, which is coupled to the sky via a large-aperture optical system. Here we present the frequency band characterization with Fourier transform spectroscopy, measurements of optical time constants, beam properties, and optical and polarization efficiencies of the detector array. The detectors have frequency bands consistent with our simulations and have high average optical efficiency which is 86, 77 and 66% for the 95, 150 and 220 GHz detectors. The time constants of the detectors are mostly between 0.5 and 5 ms. The beam is round with the correct size, and the polarization efficiency is more than 90% for most of the bolometers.

Original language	English (US)
Pages (from-to)	305-313
Number of pages	9
Journal	Journal of Low Temperature Physics
Volume	193
Issue number	3-4
DOIs	https://doi.org/10.1007/s10909-018-1935-y
State	Published - Nov 1 2018

Keywords

Beam
Cosmic microwave background
Fourier transform spectrometer
Frequency bands
Optical efficiency
Polarization
Time constant
Transition-edge sensor

ASJC Scopus subject areas

Atomic and Molecular Physics, and Optics
Materials Science(all)
Condensed Matter Physics

Online availability

10.1007/s10909-018-1935-y

Library availability

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Pan, Z., Ade, P. A. R., Ahmed, Z., Anderson, A. J., Austermann, J. E., Avva, J. S., Thakur, R. B., Bender, A. N., Benson, B. A., Carlstrom, J. E., Carter, F. W., Cecil, T., Chang, C. L., Cliche, J. F., Cukierman, A., Denison, E. V., de Haan, T., Ding, J., Dobbs, M. A., ... Young, M. R. (2018). Optical Characterization of the SPT-3G Camera. Journal of Low Temperature Physics, 193(3-4), 305-313. https://doi.org/10.1007/s10909-018-1935-y

Pan, Z, Ade, PAR, Ahmed, Z, Anderson, AJ, Austermann, JE, Avva, JS, Thakur, RB, Bender, AN, Benson, BA, Carlstrom, JE, Carter, FW, Cecil, T, Chang, CL, Cliche, JF, Cukierman, A, Denison, EV, de Haan, T, Ding, J, Dobbs, MA, Dutcher, D, Everett, W, Foster, A, Gannon, RN, Gilbert, A, Groh, JC, Halverson, NW, Harke-Hosemann, AH, Harrington, NL, Henning, JW, Hilton, GC, Holzapfel, WL, Huang, N, Irwin, KD, Jeong, OB, Jonas, M, Khaire, T, Kofman, AM, Korman, M, Kubik, D, Kuhlmann, S, Kuo, CL, Lee, AT, Lowitz, AE, Meyer, SS, Michalik, D, Montgomery, J, Nadolski, A, Natoli, T, Nguyen, H, Noble, GI, Novosad, V, Padin, S, Pearson, J, Posada, CM, Rahlin, A, Ruhl, JE, Saunders, LJ, Sayre, JT, Shirley, I, Shirokoff, E, Smecher, G, Sobrin, JA, Stark, AA, Story, KT, Suzuki, A, Tang, QY, Thompson, KL, Tucker, C, Vale, LR, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, Yoon, KW & Young, MR 2018, 'Optical Characterization of the SPT-3G Camera', Journal of Low Temperature Physics, vol. 193, no. 3-4, pp. 305-313. https://doi.org/10.1007/s10909-018-1935-y

@article{72a7c5a414be4294b1c9bc6240a6c504,

title = "Optical Characterization of the SPT-3G Camera",

abstract = "The third-generation South Pole Telescope camera is designed to measure the cosmic microwave background across three frequency bands (centered at 95, 150 and 220 GHz) with ∼ 16,000 transition-edge sensor (TES) bolometers. Each multichroic array element on a detector wafer has a broadband sinuous antenna that couples power to six TESs, one for each of the three observing bands and both polarizations, via lumped element filters. Ten detector wafers populate the detector array, which is coupled to the sky via a large-aperture optical system. Here we present the frequency band characterization with Fourier transform spectroscopy, measurements of optical time constants, beam properties, and optical and polarization efficiencies of the detector array. The detectors have frequency bands consistent with our simulations and have high average optical efficiency which is 86, 77 and 66% for the 95, 150 and 220 GHz detectors. The time constants of the detectors are mostly between 0.5 and 5 ms. The beam is round with the correct size, and the polarization efficiency is more than 90% for most of the bolometers.",

keywords = "Beam, Cosmic microwave background, Fourier transform spectrometer, Frequency bands, Optical efficiency, Polarization, Time constant, Transition-edge sensor",

author = "Z. Pan and Ade, {P. A.R.} and Z. Ahmed and Anderson, {A. J.} and Austermann, {J. E.} and Avva, {J. S.} and Thakur, {R. Basu} and Bender, {A. N.} and Benson, {B. A.} and Carlstrom, {J. E.} and Carter, {F. W.} and T. Cecil and Chang, {C. L.} and Cliche, {J. F.} and A. Cukierman and Denison, {E. V.} and {de Haan}, T. and J. Ding and Dobbs, {M. A.} and D. Dutcher and W. Everett and A. Foster and Gannon, {R. N.} and A. Gilbert and Groh, {J. C.} and Halverson, {N. W.} and Harke-Hosemann, {A. H.} and Harrington, {N. L.} and Henning, {J. W.} and Hilton, {G. C.} and Holzapfel, {W. L.} and N. Huang and Irwin, {K. D.} and Jeong, {O. B.} and M. Jonas and T. Khaire and Kofman, {A. M.} and M. Korman and D. Kubik and S. Kuhlmann and Kuo, {C. L.} and Lee, {A. T.} and Lowitz, {A. E.} and Meyer, {S. S.} and D. Michalik and J. Montgomery and A. Nadolski and T. Natoli and H. Nguyen and Noble, {G. I.} and V. Novosad and S. Padin and J. Pearson and Posada, {C. M.} and A. Rahlin and Ruhl, {J. E.} and Saunders, {L. J.} and Sayre, {J. T.} and I. Shirley and E. Shirokoff and G. Smecher and Sobrin, {J. A.} and Stark, {A. A.} and Story, {K. T.} and A. Suzuki and Tang, {Q. Y.} and Thompson, {K. L.} and C. Tucker and Vale, {L. R.} and K. Vanderlinde and Vieira, {J. D.} and G. Wang and N. Whitehorn and V. Yefremenko and Yoon, {K. W.} and Young, {M. R.}",

note = "Funding Information: authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. Funding Information: Acknowledgements The South Pole Telescope is supported by the National Science Foundation (NSF) through Grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center Grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, and the Kavli Foundation and the Gordon and Betty Moore Foundation Grant GBMF 947. Work at Argonne National Laboratory, including Laboratory Directed Research and Development support and use of the Center for Nanoscale Materials, a U.S. Department of Energy, Office of Science (DOE-OS) user facility, was supported under Contract No. DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under Contract No. DE-AC02-07CH11359. NWH acknowledges support from NSF CAREER Grant AST-0956135. The McGill Funding Information: The South Pole Telescope is supported by the National Science Foundation (NSF) through Grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center Grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, and the Kavli Foundation and the Gordon and Betty Moore Foundation Grant GBMF 947. Work at Argonne National Laboratory, including Laboratory Directed Research and Development support and use of the Center for Nanoscale Materials, a U.S. Department of Energy, Office of Science (DOE-OS) user facility, was supported under Contract No. DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under Contract No. DE-AC02-07CH11359. NWH acknowledges support from NSF CAREER Grant AST-0956135. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. Publisher Copyright: {\textcopyright} 2018, Springer Science+Business Media, LLC, part of Springer Nature.",

year = "2018",

month = nov,

day = "1",

doi = "10.1007/s10909-018-1935-y",

language = "English (US)",

volume = "193",

pages = "305--313",

journal = "Journal of Low Temperature Physics",

issn = "0022-2291",

publisher = "Springer",

number = "3-4",

}

TY - JOUR

T1 - Optical Characterization of the SPT-3G Camera

AU - Pan, Z.

AU - Ade, P. A.R.

AU - Ahmed, Z.

AU - Anderson, A. J.

AU - Austermann, J. E.

AU - Avva, J. S.

AU - Thakur, R. Basu

AU - Bender, A. N.

AU - Benson, B. A.

AU - Carlstrom, J. E.

AU - Carter, F. W.

AU - Cecil, T.

AU - Chang, C. L.

AU - Cliche, J. F.

AU - Cukierman, A.

AU - Denison, E. V.

AU - de Haan, T.

AU - Ding, J.

AU - Dobbs, M. A.

AU - Dutcher, D.

AU - Everett, W.

AU - Foster, A.

AU - Gannon, R. N.

AU - Gilbert, A.

AU - Groh, J. C.

AU - Halverson, N. W.

AU - Harke-Hosemann, A. H.

AU - Harrington, N. L.

AU - Henning, J. W.

AU - Hilton, G. C.

AU - Holzapfel, W. L.

AU - Huang, N.

AU - Irwin, K. D.

AU - Jeong, O. B.

AU - Jonas, M.

AU - Khaire, T.

AU - Kofman, A. M.

AU - Korman, M.

AU - Kubik, D.

AU - Kuhlmann, S.

AU - Kuo, C. L.

AU - Lee, A. T.

AU - Lowitz, A. E.

AU - Meyer, S. S.

AU - Michalik, D.

AU - Montgomery, J.

AU - Nadolski, A.

AU - Natoli, T.

AU - Nguyen, H.

AU - Noble, G. I.

AU - Novosad, V.

AU - Padin, S.

AU - Pearson, J.

AU - Posada, C. M.

AU - Rahlin, A.

AU - Ruhl, J. E.

AU - Saunders, L. J.

AU - Sayre, J. T.

AU - Shirley, I.

AU - Shirokoff, E.

AU - Smecher, G.

AU - Sobrin, J. A.

AU - Stark, A. A.

AU - Story, K. T.

AU - Suzuki, A.

AU - Tang, Q. Y.

AU - Thompson, K. L.

AU - Tucker, C.

AU - Vale, L. R.

AU - Vanderlinde, K.

AU - Vieira, J. D.

AU - Wang, G.

AU - Whitehorn, N.

AU - Yefremenko, V.

AU - Yoon, K. W.

AU - Young, M. R.

N1 - Funding Information: authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. Funding Information: Acknowledgements The South Pole Telescope is supported by the National Science Foundation (NSF) through Grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center Grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, and the Kavli Foundation and the Gordon and Betty Moore Foundation Grant GBMF 947. Work at Argonne National Laboratory, including Laboratory Directed Research and Development support and use of the Center for Nanoscale Materials, a U.S. Department of Energy, Office of Science (DOE-OS) user facility, was supported under Contract No. DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under Contract No. DE-AC02-07CH11359. NWH acknowledges support from NSF CAREER Grant AST-0956135. The McGill Funding Information: The South Pole Telescope is supported by the National Science Foundation (NSF) through Grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center Grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, and the Kavli Foundation and the Gordon and Betty Moore Foundation Grant GBMF 947. Work at Argonne National Laboratory, including Laboratory Directed Research and Development support and use of the Center for Nanoscale Materials, a U.S. Department of Energy, Office of Science (DOE-OS) user facility, was supported under Contract No. DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under Contract No. DE-AC02-07CH11359. NWH acknowledges support from NSF CAREER Grant AST-0956135. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. Publisher Copyright: © 2018, Springer Science+Business Media, LLC, part of Springer Nature.

PY - 2018/11/1

Y1 - 2018/11/1

N2 - The third-generation South Pole Telescope camera is designed to measure the cosmic microwave background across three frequency bands (centered at 95, 150 and 220 GHz) with ∼ 16,000 transition-edge sensor (TES) bolometers. Each multichroic array element on a detector wafer has a broadband sinuous antenna that couples power to six TESs, one for each of the three observing bands and both polarizations, via lumped element filters. Ten detector wafers populate the detector array, which is coupled to the sky via a large-aperture optical system. Here we present the frequency band characterization with Fourier transform spectroscopy, measurements of optical time constants, beam properties, and optical and polarization efficiencies of the detector array. The detectors have frequency bands consistent with our simulations and have high average optical efficiency which is 86, 77 and 66% for the 95, 150 and 220 GHz detectors. The time constants of the detectors are mostly between 0.5 and 5 ms. The beam is round with the correct size, and the polarization efficiency is more than 90% for most of the bolometers.

AB - The third-generation South Pole Telescope camera is designed to measure the cosmic microwave background across three frequency bands (centered at 95, 150 and 220 GHz) with ∼ 16,000 transition-edge sensor (TES) bolometers. Each multichroic array element on a detector wafer has a broadband sinuous antenna that couples power to six TESs, one for each of the three observing bands and both polarizations, via lumped element filters. Ten detector wafers populate the detector array, which is coupled to the sky via a large-aperture optical system. Here we present the frequency band characterization with Fourier transform spectroscopy, measurements of optical time constants, beam properties, and optical and polarization efficiencies of the detector array. The detectors have frequency bands consistent with our simulations and have high average optical efficiency which is 86, 77 and 66% for the 95, 150 and 220 GHz detectors. The time constants of the detectors are mostly between 0.5 and 5 ms. The beam is round with the correct size, and the polarization efficiency is more than 90% for most of the bolometers.

KW - Beam

KW - Cosmic microwave background

KW - Fourier transform spectrometer

KW - Frequency bands

KW - Optical efficiency

KW - Polarization

KW - Time constant

KW - Transition-edge sensor

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UR - http://www.scopus.com/inward/citedby.url?scp=85046719061&partnerID=8YFLogxK

U2 - 10.1007/s10909-018-1935-y

DO - 10.1007/s10909-018-1935-y

M3 - Article

AN - SCOPUS:85046719061

SN - 0022-2291

VL - 193

SP - 305

EP - 313

JO - Journal of Low Temperature Physics

JF - Journal of Low Temperature Physics

IS - 3-4

ER -

Optical Characterization of the SPT-3G Camera

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