The Design and Integrated Performance of SPT-3G

J. A. Sobrin; A. J. Anderson; A. N. Bender; B. A. Benson; D. Dutcher; A. Foster; N. Goeckner-Wald; J. Montgomery; A. Nadolski; A. Rahlin; P. A.R. Ade; Z. Ahmed; E. Anderes; M. Archipley; J. E. Austermann; J. S. Avva; K. Aylor; L. Balkenhol; P. S. Barry; R. Basu Thakur; K. Benabed; F. Bianchini; L. E. Bleem; F. R. Bouchet; L. Bryant; K. Byrum; J. E. Carlstrom; F. W. Carter; T. W. Cecil; C. L. Chang; P. Chaubal; G. Chen; H. M. Cho; T. L. Chou; J. F. Cliche; T. M. Crawford; A. Cukierman; C. Daley; T. De Haan; E. V. Denison; K. Dibert; J. Ding; M. A. Dobbs; W. Everett; C. Feng; K. R. Ferguson; J. Fu; S. Galli; A. E. Gambrel; R. W. Gardner; R. Gualtieri; S. Guns; N. Gupta; R. Guyser; N. W. Halverson; A. H. Harke-Hosemann; N. L. Harrington; J. W. Henning; G. C. Hilton; E. Hivon; G. P. Holder; W. L. Holzapfel; J. C. Hood; D. Howe; N. Huang; K. D. Irwin; O. B. Jeong; M. Jonas; A. Jones; T. S. Khaire; L. Knox; A. M. Kofman; M. Korman; D. L. Kubik; S. Kuhlmann; C. L. Kuo; A. T. Lee; E. M. Leitch; A. E. Lowitz; C. Lu; S. S. Meyer; D. Michalik; M. Millea; T. Natoli; H. Nguyen; G. I. Noble; V. Novosad; Y. Omori; S. Padin; Z. Pan; P. Paschos; J. Pearson; C. M. Posada; K. Prabhu; W. Quan; C. L. Reichardt; D. Riebel; B. Riedel; M. Rouble; J. E. Ruhl; B. Saliwanchik; J. T. Sayre; E. Schiappucci; E. Shirokoff; G. Smecher; A. A. Stark; J. Stephen; K. T. Story; A. Suzuki; C. Tandoi; K. L. Thompson; B. Thorne; C. Tucker; C. Umilta; L. R. Vale; K. Vanderlinde; J. D. Vieira; G. Wang; N. Whitehorn; W. L.K. Wu; V. Yefremenko; K. W. Yoon; M. R. Young

doi:10.3847/1538-4365/ac374f

The Design and Integrated Performance of SPT-3G

J. A. Sobrin, A. J. Anderson, A. N. Bender, B. A. Benson, D. Dutcher, A. Foster, N. Goeckner-Wald, J. Montgomery, A. Nadolski, A. Rahlin, P. A.R. Ade, Z. Ahmed, E. Anderes, M. Archipley, J. E. Austermann, J. S. Avva, K. Aylor, L. Balkenhol, P. S. Barry, R. Basu ThakurK. Benabed, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. M. Cho, T. L. Chou, J. F. Cliche, T. M. Crawford, A. Cukierman, C. Daley, T. De Haan, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, A. E. Gambrel, R. W. Gardner, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, N. Huang, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C. L. Kuo, A. T. Lee, E. M. Leitch, A. E. Lowitz, C. Lu, S. S. Meyer, D. Michalik, M. Millea, T. Natoli, H. Nguyen, G. I. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, J. Pearson, C. M. Posada, K. Prabhu, W. Quan, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. Saliwanchik, J. T. Sayre, E. Schiappucci, E. Shirokoff, G. Smecher, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, K. Vanderlinde, J. D. Vieira, G. Wang, N. Whitehorn, W. L.K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young

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

Abstract

SPT-3G is the third survey receiver operating on the South Pole Telescope dedicated to high-resolution observations of the cosmic microwave background (CMB). Sensitive measurements of the temperature and polarization anisotropies of the CMB provide a powerful data set for constraining cosmology. Additionally, CMB surveys with arcminute-scale resolution are capable of detecting galaxy clusters, millimeter-wave bright galaxies, and a variety of transient phenomena. The SPT-3G instrument provides a significant improvement in mapping speed over its predecessors, SPT-SZ and SPTpol. The broadband optics design of the instrument achieves a 430 mm diameter image plane across observing bands of 95, 150, and 220 GHz, with 1.2′ FWHM beam response at 150 GHz. In the receiver, this image plane is populated with 2690 dual-polarization, trichroic pixels ( 1/416,000 detectors) read out using a 68× digital frequency-domain multiplexing readout system. In 2018, SPT-3G began a multiyear survey of 1500 deg2 of the southern sky. We summarize the unique optical, cryogenic, detector, and readout technologies employed in SPT-3G, and we report on the integrated performance of the instrument.

Original language	English (US)
Article number	42
Journal	Astrophysical Journal, Supplement Series
Volume	258
Issue number	2
DOIs	https://doi.org/10.3847/1538-4365/ac374f
State	Published - 2022

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4365/ac374f

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Sobrin, J. A., Anderson, A. J., Bender, A. N., Benson, B. A., Dutcher, D., Foster, A., Goeckner-Wald, N., Montgomery, J., Nadolski, A., Rahlin, A., Ade, P. A. R., Ahmed, Z., Anderes, E., Archipley, M., Austermann, J. E., Avva, J. S., Aylor, K., Balkenhol, L., Barry, P. S., ... Young, M. R. (2022). The Design and Integrated Performance of SPT-3G. Astrophysical Journal, Supplement Series, 258(2), [42]. https://doi.org/10.3847/1538-4365/ac374f

Sobrin, JA, Anderson, AJ, Bender, AN, Benson, BA, Dutcher, D, Foster, A, Goeckner-Wald, N, Montgomery, J, Nadolski, A, Rahlin, A, Ade, PAR, Ahmed, Z, Anderes, E, Archipley, M, Austermann, JE, Avva, JS, Aylor, K, Balkenhol, L, Barry, PS, Thakur, RB, Benabed, K, Bianchini, F, Bleem, LE, Bouchet, FR, Bryant, L, Byrum, K, Carlstrom, JE, Carter, FW, Cecil, TW, Chang, CL, Chaubal, P, Chen, G, Cho, HM, Chou, TL, Cliche, JF, Crawford, TM, Cukierman, A, Daley, C, Haan, TD, Denison, EV, Dibert, K, Ding, J, Dobbs, MA, Everett, W, Feng, C, Ferguson, KR, Fu, J, Galli, S, Gambrel, AE, Gardner, RW, Gualtieri, R, Guns, S, Gupta, N, Guyser, R, Halverson, NW, Harke-Hosemann, AH, Harrington, NL, Henning, JW, Hilton, GC, Hivon, E, Holder, GP, Holzapfel, WL, Hood, JC, Howe, D, Huang, N, Irwin, KD, Jeong, OB, Jonas, M, Jones, A, Khaire, TS, Knox, L, Kofman, AM, Korman, M, Kubik, DL, Kuhlmann, S, Kuo, CL, Lee, AT, Leitch, EM, Lowitz, AE, Lu, C, Meyer, SS, Michalik, D, Millea, M, Natoli, T, Nguyen, H, Noble, GI, Novosad, V, Omori, Y, Padin, S, Pan, Z, Paschos, P, Pearson, J, Posada, CM, Prabhu, K, Quan, W, Reichardt, CL, Riebel, D, Riedel, B, Rouble, M, Ruhl, JE, Saliwanchik, B, Sayre, JT, Schiappucci, E, Shirokoff, E, Smecher, G, Stark, AA, Stephen, J, Story, KT, Suzuki, A, Tandoi, C, Thompson, KL, Thorne, B, Tucker, C, Umilta, C, Vale, LR, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, Yefremenko, V, Yoon, KW & Young, MR 2022, 'The Design and Integrated Performance of SPT-3G', Astrophysical Journal, Supplement Series, vol. 258, no. 2, 42. https://doi.org/10.3847/1538-4365/ac374f

@article{1d368eeb0c284fcab62f1be76b3f5a16,

title = "The Design and Integrated Performance of SPT-3G",

abstract = "SPT-3G is the third survey receiver operating on the South Pole Telescope dedicated to high-resolution observations of the cosmic microwave background (CMB). Sensitive measurements of the temperature and polarization anisotropies of the CMB provide a powerful data set for constraining cosmology. Additionally, CMB surveys with arcminute-scale resolution are capable of detecting galaxy clusters, millimeter-wave bright galaxies, and a variety of transient phenomena. The SPT-3G instrument provides a significant improvement in mapping speed over its predecessors, SPT-SZ and SPTpol. The broadband optics design of the instrument achieves a 430 mm diameter image plane across observing bands of 95, 150, and 220 GHz, with 1.2′ FWHM beam response at 150 GHz. In the receiver, this image plane is populated with 2690 dual-polarization, trichroic pixels ( 1/416,000 detectors) read out using a 68× digital frequency-domain multiplexing readout system. In 2018, SPT-3G began a multiyear survey of 1500 deg2 of the southern sky. We summarize the unique optical, cryogenic, detector, and readout technologies employed in SPT-3G, and we report on the integrated performance of the instrument.",

author = "Sobrin, {J. A.} and Anderson, {A. J.} and Bender, {A. N.} and Benson, {B. A.} and D. Dutcher and A. Foster and N. Goeckner-Wald and J. Montgomery and A. Nadolski and A. Rahlin and Ade, {P. A.R.} and Z. Ahmed and E. Anderes and M. Archipley and Austermann, {J. E.} and Avva, {J. S.} and K. Aylor and L. Balkenhol and Barry, {P. S.} and Thakur, {R. Basu} and K. Benabed and F. Bianchini and Bleem, {L. E.} and Bouchet, {F. R.} and L. Bryant and K. Byrum and Carlstrom, {J. E.} and Carter, {F. W.} and Cecil, {T. W.} and Chang, {C. L.} and P. Chaubal and G. Chen and Cho, {H. M.} and Chou, {T. L.} and Cliche, {J. F.} and Crawford, {T. M.} and A. Cukierman and C. Daley and Haan, {T. De} and Denison, {E. V.} and K. Dibert and J. Ding and Dobbs, {M. A.} and W. Everett and C. Feng and Ferguson, {K. R.} and J. Fu and S. Galli and Gambrel, {A. E.} and Gardner, {R. W.} and R. Gualtieri and S. Guns and N. Gupta and R. Guyser and Halverson, {N. W.} and Harke-Hosemann, {A. H.} and Harrington, {N. L.} and Henning, {J. W.} and Hilton, {G. C.} and E. Hivon and Holder, {G. P.} and Holzapfel, {W. L.} and Hood, {J. C.} and D. Howe and N. Huang and Irwin, {K. D.} and Jeong, {O. B.} and M. Jonas and A. Jones and Khaire, {T. S.} and L. Knox and Kofman, {A. M.} and M. Korman and Kubik, {D. L.} and S. Kuhlmann and Kuo, {C. L.} and Lee, {A. T.} and Leitch, {E. M.} and Lowitz, {A. E.} and C. Lu and Meyer, {S. S.} and D. Michalik and M. Millea and T. Natoli and H. Nguyen and Noble, {G. I.} and V. Novosad and Y. Omori and S. Padin and Z. Pan and P. Paschos and J. Pearson and Posada, {C. M.} and K. Prabhu and W. Quan and Reichardt, {C. L.} and D. Riebel and B. Riedel and M. Rouble and Ruhl, {J. E.} and B. Saliwanchik and Sayre, {J. T.} and E. Schiappucci and E. Shirokoff and G. Smecher and Stark, {A. A.} and J. Stephen and Story, {K. T.} and A. Suzuki and C. Tandoi and Thompson, {K. L.} and B. Thorne and C. Tucker and C. Umilta and Vale, {L. R.} and K. Vanderlinde and Vieira, {J. D.} and G. Wang and N. Whitehorn and Wu, {W. L.K.} and V. Yefremenko and Yoon, {K. W.} and Young, {M. R.}",

note = "Funding Information: The South Pole Telescope program is supported by the National Science Foundation (NSF) through grants PLR-1248097 and OPP-1852617. 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. Argonne National Laboratory{\textquoteright}s work was supported by the U.S. Department of Energy, Office of High Energy Physics, under contract DE-AC02-06CH11357. This work was performed, in part, at the Center for Nanoscale Materials, a U.S. Department of Energy Office of Science User Facility, and supported by the U.S. Department of Energy, Office of Science, under Contract No. DE-AC02-06CH11357. We acknowledge R. Divan, L. Stan, C.S. Miller, and V. Kutepova for supporting our work in the Argonne Center for Nanoscale Materials. 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. N.W.H. 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 the Fonds de recherche du Qu{\'e}bec Nature et technologies. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics under Award Number DE-SC-0015640. M.A. and J.V. acknowledge support from the Center for AstroPhysical Surveys at the National Center for Supercomputing Applications in Urbana, IL. J.V. acknowledges support from the Sloan Foundation. Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",

year = "2022",

doi = "10.3847/1538-4365/ac374f",

language = "English (US)",

volume = "258",

journal = "Astrophysical Journal, Supplement Series",

issn = "0067-0049",

publisher = "IOP Publishing Ltd.",

number = "2",

}

TY - JOUR

T1 - The Design and Integrated Performance of SPT-3G

AU - Sobrin, J. A.

AU - Anderson, A. J.

AU - Bender, A. N.

AU - Benson, B. A.

AU - Dutcher, D.

AU - Foster, A.

AU - Goeckner-Wald, N.

AU - Montgomery, J.

AU - Nadolski, A.

AU - Rahlin, A.

AU - Ade, P. A.R.

AU - Ahmed, Z.

AU - Anderes, E.

AU - Archipley, M.

AU - Austermann, J. E.

AU - Avva, J. S.

AU - Aylor, K.

AU - Balkenhol, L.

AU - Barry, P. S.

AU - Thakur, R. Basu

AU - Benabed, K.

AU - Bianchini, F.

AU - Bleem, L. E.

AU - Bouchet, F. R.

AU - Bryant, L.

AU - Byrum, K.

AU - Carlstrom, J. E.

AU - Carter, F. W.

AU - Cecil, T. W.

AU - Chang, C. L.

AU - Chaubal, P.

AU - Chen, G.

AU - Cho, H. M.

AU - Chou, T. L.

AU - Cliche, J. F.

AU - Crawford, T. M.

AU - Cukierman, A.

AU - Daley, C.

AU - Haan, T. De

AU - Denison, E. V.

AU - Dibert, K.

AU - Ding, J.

AU - Dobbs, M. A.

AU - Everett, W.

AU - Feng, C.

AU - Ferguson, K. R.

AU - Fu, J.

AU - Galli, S.

AU - Gambrel, A. E.

AU - Gardner, R. W.

AU - Gualtieri, R.

AU - Guns, S.

AU - Gupta, N.

AU - Guyser, R.

AU - Halverson, N. W.

AU - Harke-Hosemann, A. H.

AU - Harrington, N. L.

AU - Henning, J. W.

AU - Hilton, G. C.

AU - Hivon, E.

AU - Holder, G. P.

AU - Holzapfel, W. L.

AU - Hood, J. C.

AU - Howe, D.

AU - Huang, N.

AU - Irwin, K. D.

AU - Jeong, O. B.

AU - Jonas, M.

AU - Jones, A.

AU - Khaire, T. S.

AU - Knox, L.

AU - Kofman, A. M.

AU - Korman, M.

AU - Kubik, D. L.

AU - Kuhlmann, S.

AU - Kuo, C. L.

AU - Lee, A. T.

AU - Leitch, E. M.

AU - Lowitz, A. E.

AU - Lu, C.

AU - Meyer, S. S.

AU - Michalik, D.

AU - Millea, M.

AU - Natoli, T.

AU - Nguyen, H.

AU - Noble, G. I.

AU - Novosad, V.

AU - Omori, Y.

AU - Padin, S.

AU - Pan, Z.

AU - Paschos, P.

AU - Pearson, J.

AU - Posada, C. M.

AU - Prabhu, K.

AU - Quan, W.

AU - Reichardt, C. L.

AU - Riebel, D.

AU - Riedel, B.

AU - Rouble, M.

AU - Ruhl, J. E.

AU - Saliwanchik, B.

AU - Sayre, J. T.

AU - Schiappucci, E.

AU - Shirokoff, E.

AU - Smecher, G.

AU - Stark, A. A.

AU - Stephen, J.

AU - Story, K. T.

AU - Suzuki, A.

AU - Tandoi, C.

AU - Thompson, K. L.

AU - Thorne, B.

AU - Tucker, C.

AU - Umilta, C.

AU - Vale, L. R.

AU - Vanderlinde, K.

AU - Vieira, J. D.

AU - Wang, G.

AU - Whitehorn, N.

AU - Wu, W. L.K.

AU - Yefremenko, V.

AU - Yoon, K. W.

AU - Young, M. R.

N1 - Funding Information: The South Pole Telescope program is supported by the National Science Foundation (NSF) through grants PLR-1248097 and OPP-1852617. 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. Argonne National Laboratory’s work was supported by the U.S. Department of Energy, Office of High Energy Physics, under contract DE-AC02-06CH11357. This work was performed, in part, at the Center for Nanoscale Materials, a U.S. Department of Energy Office of Science User Facility, and supported by the U.S. Department of Energy, Office of Science, under Contract No. DE-AC02-06CH11357. We acknowledge R. Divan, L. Stan, C.S. Miller, and V. Kutepova for supporting our work in the Argonne Center for Nanoscale Materials. 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. N.W.H. 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 the Fonds de recherche du Québec Nature et technologies. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics under Award Number DE-SC-0015640. M.A. and J.V. acknowledge support from the Center for AstroPhysical Surveys at the National Center for Supercomputing Applications in Urbana, IL. J.V. acknowledges support from the Sloan Foundation. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

PY - 2022

Y1 - 2022

N2 - SPT-3G is the third survey receiver operating on the South Pole Telescope dedicated to high-resolution observations of the cosmic microwave background (CMB). Sensitive measurements of the temperature and polarization anisotropies of the CMB provide a powerful data set for constraining cosmology. Additionally, CMB surveys with arcminute-scale resolution are capable of detecting galaxy clusters, millimeter-wave bright galaxies, and a variety of transient phenomena. The SPT-3G instrument provides a significant improvement in mapping speed over its predecessors, SPT-SZ and SPTpol. The broadband optics design of the instrument achieves a 430 mm diameter image plane across observing bands of 95, 150, and 220 GHz, with 1.2′ FWHM beam response at 150 GHz. In the receiver, this image plane is populated with 2690 dual-polarization, trichroic pixels ( 1/416,000 detectors) read out using a 68× digital frequency-domain multiplexing readout system. In 2018, SPT-3G began a multiyear survey of 1500 deg2 of the southern sky. We summarize the unique optical, cryogenic, detector, and readout technologies employed in SPT-3G, and we report on the integrated performance of the instrument.

AB - SPT-3G is the third survey receiver operating on the South Pole Telescope dedicated to high-resolution observations of the cosmic microwave background (CMB). Sensitive measurements of the temperature and polarization anisotropies of the CMB provide a powerful data set for constraining cosmology. Additionally, CMB surveys with arcminute-scale resolution are capable of detecting galaxy clusters, millimeter-wave bright galaxies, and a variety of transient phenomena. The SPT-3G instrument provides a significant improvement in mapping speed over its predecessors, SPT-SZ and SPTpol. The broadband optics design of the instrument achieves a 430 mm diameter image plane across observing bands of 95, 150, and 220 GHz, with 1.2′ FWHM beam response at 150 GHz. In the receiver, this image plane is populated with 2690 dual-polarization, trichroic pixels ( 1/416,000 detectors) read out using a 68× digital frequency-domain multiplexing readout system. In 2018, SPT-3G began a multiyear survey of 1500 deg2 of the southern sky. We summarize the unique optical, cryogenic, detector, and readout technologies employed in SPT-3G, and we report on the integrated performance of the instrument.

UR - http://www.scopus.com/inward/record.url?scp=85125835916&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85125835916&partnerID=8YFLogxK

U2 - 10.3847/1538-4365/ac374f

DO - 10.3847/1538-4365/ac374f

M3 - Article

AN - SCOPUS:85125835916

SN - 0067-0049

VL - 258

JO - Astrophysical Journal, Supplement Series

JF - Astrophysical Journal, Supplement Series

IS - 2

M1 - 42

ER -

The Design and Integrated Performance of SPT-3G

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