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Journal of Low Temperature Physics

, Volume 193, Issue 5–6, pp 703–711 | Cite as

Fabrication of Detector Arrays for the SPT-3G Receiver

  • C. M. Posada
  • 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
  • R. Divan
  • 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
  • C. S. Miller
  • J. Montgomery
  • A. Nadolski
  • T. Natoli
  • H. Nguyen
  • G. I. Noble
  • V. Novosad
  • S. Padin
  • Z. Pan
  • J. Pearson
  • A. Rahlin
  • J. E. Ruhl
  • L. J. Saunders
  • J. T. Sayre
  • I. Shirley
  • E. Shirokoff
  • G. Smecher
  • J. A. Sobrin
  • L. Stan
  • 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
Article

Abstract

The South Pole Telescope third-generation (SPT-3G) receiver was installed during the austral summer of 2016–2017. It is designed to measure the cosmic microwave background across three frequency bands centered at 95, 150, and 220 GHz. The SPT-3G receiver has ten focal plane modules, each with 269 pixels. Each pixel features a broadband sinuous antenna coupled to a niobium microstrip transmission line. In-line filters define the desired band-passes before the signal is coupled to six bolometers with Ti/Au/Ti/Au transition edge sensors (three bands \(\times \) two polarizations). In total, the SPT-3G receiver is composed of  16,000 detectors, which are read out using a 68\(\times \) frequency-domain multiplexing scheme. In this paper, we present the process employed in fabricating the detector arrays.

Keywords

Bolometers Cosmic microwave background TES detectors Multichroic sensors SPT-3G 

Notes

Acknowledgements

The South Pole Telescope is supported by the National Science Foundation through Grant PLR-1248097. This work was also supported in part by the US Department of Energy under Contract Number DE-AC02-76SF00515. Work at Argonne National Laboratory is supported by UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a US Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. Use of the Center for Nanoscale Materials, an Office of Science user facility, was supported by the US Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-06CH11357. 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, the Kavli Foundation and the Gordon and Betty Moore Foundation Grant GBMF 947. BB is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the US Department of Energy. NWH acknowledges additional support from NSF CAREER Grant AST-0906135. JWH is supported by the NSF under Award No. AST-1402161. 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.

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Copyright information

© This is a U.S. government work and its text is not subject to copyright protection in the United States; however, its text may be subject to foreign copyright protection 2018

Authors and Affiliations

  • C. M. Posada
    • 1
  • P. A. R. Ade
    • 2
  • Z. Ahmed
    • 3
    • 4
    • 5
  • A. J. Anderson
    • 6
    • 7
  • J. E. Austermann
    • 8
  • J. S. Avva
    • 9
  • R. Basu Thakur
    • 7
  • A. N. Bender
    • 7
    • 10
  • B. A. Benson
    • 6
    • 7
    • 11
  • J. E. Carlstrom
    • 7
    • 10
    • 11
    • 12
    • 13
  • F. W. Carter
    • 7
    • 10
  • T. Cecil
    • 10
  • C. L. Chang
    • 7
    • 10
    • 11
  • J. F. Cliche
    • 14
  • A. Cukierman
    • 9
  • E. V. Denison
    • 8
  • T. de Haan
    • 9
  • J. Ding
    • 1
  • R. Divan
    • 15
  • M. A. Dobbs
    • 14
    • 16
  • D. Dutcher
    • 7
    • 13
  • W. Everett
    • 17
  • A. Foster
    • 18
  • R. N. Gannon
    • 1
  • A. Gilbert
    • 14
  • J. C. Groh
    • 9
  • N. W. Halverson
    • 17
    • 19
  • A. H. Harke-Hosemann
    • 10
    • 20
  • N. L. Harrington
    • 9
  • J. W. Henning
    • 7
  • G. C. Hilton
    • 8
  • W. L. Holzapfel
    • 9
  • N. Huang
    • 9
  • K. D. Irwin
    • 3
    • 4
    • 5
  • O. B. Jeong
    • 9
  • M. Jonas
    • 6
  • T. Khaire
    • 1
  • A. M. Kofman
    • 20
    • 21
  • M. Korman
    • 18
  • D. Kubik
    • 6
  • S. Kuhlmann
    • 10
  • C. L. Kuo
    • 3
    • 4
    • 5
  • A. T. Lee
    • 9
    • 22
  • A. E. Lowitz
    • 7
  • S. S. Meyer
    • 7
    • 11
    • 12
    • 13
  • D. Michalik
    • 11
  • C. S. Miller
    • 15
  • J. Montgomery
    • 14
  • A. Nadolski
    • 20
  • T. Natoli
    • 23
  • H. Nguyen
    • 6
  • G. I. Noble
    • 14
  • V. Novosad
    • 1
  • S. Padin
    • 7
  • Z. Pan
    • 7
    • 13
  • J. Pearson
    • 1
  • A. Rahlin
    • 6
    • 7
  • J. E. Ruhl
    • 18
  • L. J. Saunders
    • 7
    • 10
  • J. T. Sayre
    • 17
  • I. Shirley
    • 9
  • E. Shirokoff
    • 7
    • 11
  • G. Smecher
    • 24
  • J. A. Sobrin
    • 7
    • 13
  • L. Stan
    • 15
  • A. A. Stark
    • 25
  • K. T. Story
    • 3
    • 4
  • A. Suzuki
    • 9
    • 22
  • Q. Y. Tang
    • 7
    • 11
  • K. L. Thompson
    • 3
    • 4
    • 5
  • C. Tucker
    • 2
  • L. R. Vale
    • 8
  • K. Vanderlinde
    • 23
    • 26
  • J. D. Vieira
    • 20
    • 21
  • G. Wang
    • 10
  • N. Whitehorn
    • 9
    • 27
  • V. Yefremenko
    • 10
  • K. W. Yoon
    • 3
    • 4
    • 5
  • M. R. Young
    • 26
  1. 1.Material Science DivisionArgonne National LaboratoryArgonneUSA
  2. 2.School of Physics and AstronomyCardiff UniversityCardiffUK
  3. 3.Kavli Institute for Particle Astrophysics and CosmologyStanford UniversityStanfordUSA
  4. 4.Department of PhysicsStanford UniversityStanfordUSA
  5. 5.SLAC National Accelerator LaboratoryMenlo ParkUSA
  6. 6.Fermi National Accelerator Laboratory, MS209BataviaUSA
  7. 7.Kavli Institute for Cosmological PhysicsUniversity of ChicagoChicagoUSA
  8. 8.National Institute of Standards and TechnologyBoulderUSA
  9. 9.Department of PhysicsUniversity of CaliforniaBerkeleyUSA
  10. 10.High-Energy Physics DivisionArgonne National LaboratoryArgonneUSA
  11. 11.Department of Astronomy and AstrophysicsUniversity of ChicagoChicagoUSA
  12. 12.Enrico Fermi InstituteUniversity of ChicagoChicagoUSA
  13. 13.Department of PhysicsUniversity of ChicagoChicagoUSA
  14. 14.Department of PhysicsMcGill UniversityMontrealCanada
  15. 15.Argonne National LaboratoryCenter for Nanoscale MaterialsArgonneUSA
  16. 16.CIFAR Program in Cosmology and GravityCanadian Institute for Advanced ResearchTorontoCanada
  17. 17.CASA, Department of Astrophysical and Planetary SciencesUniversity of ColoradoBoulderUSA
  18. 18.Physics DepartmentCase Western Reserve UniversityClevelandUSA
  19. 19.Department of PhysicsUniversity of ColoradoBoulderUSA
  20. 20.Astronomy DepartmentUniversity of IllinoisUrbanaUSA
  21. 21.Department of PhysicsUniversity of IllinoisUrbanaUSA
  22. 22.Physics DivisionLawrence Berkeley National LaboratoryBerkeleyUSA
  23. 23.Dunlap Institute for Astronomy and AstrophysicsUniversity of TorontoTorontoCanada
  24. 24.Three-Speed Logic, Inc.VancouverCanada
  25. 25.Harvard-Smithsonian Center for AstrophysicsCambridgeUSA
  26. 26.Department of Astronomy and AstrophysicsUniversity of TorontoTorontoCanada
  27. 27.Department of Physics and AstronomyUniversity of CaliforniaLos AngelesUSA

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