The Design and Integrated Performance of SPT-3G

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

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 (∼16,000 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.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 June 18; revised 2021 October 18; accepted 2021 November 5; published 2022 February 9. 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. Facility: Amundsen–Scott South Pole Station. - Software: IPython (Perez & Granger 2007), LMFIT (Newville et al. 2014), Matplotlib (Hunter 2007), NumPy (van der Walt et al. 2011), Pandas (McKinney 2010), and SciPy (Jones et al. 2001).

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