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Proceedings Paper

Integrated performance of a frequency domain multiplexing readout in the SPT-3G receiver
Author(s): A. N. Bender; P. A. R. Ade; A. J. Anderson; J. Avva; Z. Ahmed; K. Arnold; J. E. Austermann; R. Basu Thakur; B. A. Benson; L. E. Bleem; K. Byrum; J. E. Carlstrom; F. W. Carter; C. L. Chang; H. M. Cho; J. F. Cliche; T. M. Crawford; A. Cukierman; D. A. Czaplewski; J. Ding; R. Divan; T. de Haan; M. A. Dobbs; D. Dutcher; W. Everett; A. Gilbert; J. C. Groh; R. Guyser; N. W. Halverson; A. Harke-Hosemann; N. L. Harrington; K. Hattori; J. W. Henning; G. C. Hilton; W. L. Holzapfel; N. Huang; K. D. Irwin; O. Jeong; T. Khaire; M. Korman; D. Kubik; C. L. Kuo; A. T. Lee; E. M. Leitch; S. Lendinez; S. S. Meyer; C. S. Miller; J. Montgomery; A. Nadolski; T. Natoli; H. Nguyen; V. Novosad; S. Padin; Z. Pan; J. Pearson; C. M. Posada; A. Rahlin; C. L. Reichardt; J. E. Ruhl; B. R. Saliwanchik; J. T. Sayre; J. A. Shariff; Ian Shirley; E. Shirokoff; G. Smecher; J. Sobrin; L. Stan; A. A. Stark; K. Story; A. Suzuki; Q. Y. Tang; K. L. Thompson; C. Tucker; K. Vanderlinde; J. D. Vieira; G. Wang; N. Whitehorn; V. Yefremenko; K. W. Yoon
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Paper Abstract

The third generation receiver for the South Pole Telescope, SPT-3G, will make extremely deep, arcminuteresolution maps of the temperature and polarization of the cosmic microwave background. The SPT-3G maps will enable studies of the B-mode polarization signature, constraining primordial gravitational waves as well as the effect of massive neutrinos on structure formation in the late universe. The SPT-3G receiver will achieve exceptional sensitivity through a focal plane of ~16,000 transition-edge sensor bolometers, an order of magnitude more than the current SPTpol receiver. SPT-3G uses a frequency domain multiplexing (fMux) scheme to read out the focal plane, combining the signals from 64 bolometers onto a single pair of wires. The fMux readout facilitates the large number of detectors in the SPT-3G focal plane by limiting the thermal load due to readout wiring on the 250 millikelvin cryogenic stage. A second advantage of the fMux system is that the operation of each bolometer can be optimized. In addition to these benefits, the fMux readout introduces new challenges into the design and operation of the receiver. The bolometers are operated at a range of frequencies up to 5 MHz, requiring control of stray reactances over a large bandwidth. Additionally, crosstalk between multiplexed detectors will inject large false signals into the data if not adequately mitigated. SPT-3G is scheduled to deploy to the South Pole Telescope in late 2016. Here, we present the pre-deployment performance of the fMux readout system with the SPT-3G focal plane.

Paper Details

Date Published: 20 July 2016
PDF: 11 pages
Proc. SPIE 9914, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, 99141D (20 July 2016); doi: 10.1117/12.2232146
Show Author Affiliations
A. N. Bender, Argonne National Lab. (United States)
Kavli Institute for Cosmological Physics (United States)
P. A. R. Ade, Cardiff Univ. (United Kingdom)
A. J. Anderson, Fermi National Accelerator Lab. (United States)
Kavli Institute for Cosmological Physics (United States)
J. Avva, Univ. of California, Berkeley (United States)
Z. Ahmed, Kavli Institute for Particle Astrophysics & Cosmology (United States)
Stanford Univ. (United States)
SLAC National Accelerator Lab. (United States)
K. Arnold, Univ. of Wisconsin-Madison (United States)
J. E. Austermann, NIST Quantum Devices Group (United States)
R. Basu Thakur, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
B. A. Benson, Fermi National Accelerator Lab. (United States)
Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
L. E. Bleem, Argonne National Lab. (United States)
Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
K. Byrum, Argonne National Lab. (United States)
J. E. Carlstrom, Kavli Institute for Cosmological Physics (United States)
The Enrico Fermi Institute (United States)
Argonne National Lab. and The Univ. of Chicago (United States)
F. W. Carter, Argonne National Lab. (United States)
Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
C. L. Chang, Argonne National Lab. (United States)
Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
H. M. Cho, SLAC National Accelerator Lab. (United States)
J. F. Cliche, McGill Univ. (Canada)
T. M. Crawford, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
A. Cukierman, Univ. of California, Berkeley (United States)
D. A. Czaplewski, Argonne National Lab. (United States)
J. Ding, Argonne National Lab. (United States)
R. Divan, Argonne National Lab. (United States)
T. de Haan, Univ. of California, Berkeley (United States)
M. A. Dobbs, McGill Univ. (Canada)
Canadian Institute for Advanced Research (Canada)
D. Dutcher, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
W. Everett, Univ. of Colorado at Boulder (United States)
A. Gilbert, McGill Univ. (Canada)
J. C. Groh, Univ. of California, Berkeley (United States)
R. Guyser, Univ. of Illinois at Urbana-Champaign (United States)
N. W. Halverson, Univ. of Colorado at Boulder (United States)
A. Harke-Hosemann, Univ. of Illinois at Urbana-Champaign (United States)
N. L. Harrington, Univ. of California, Berkeley (United States)
K. Hattori, High Energy Accelerator Research Organization, KEK (Japan)
J. W. Henning, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
G. C. Hilton, National Institute of Standards and Technology (United States)
W. L. Holzapfel, Univ. of California, Berkeley (United States)
N. Huang, Univ. of California, Berkeley (United States)
K. D. Irwin, Kavli Institute for Particle Astrophysics & Cosmology (United States)
Stanford Univ. (United States)
SLAC National Accelerator Lab. (United States)
O. Jeong, Univ. of California, Berkeley (United States)
T. Khaire, Argonne National Lab. (United States)
M. Korman, Univ. of California, Davis (United States)
D. Kubik, Fermi National Accelerator Lab. (United States)
C. L. Kuo, Kavli Institute for Particle Astrophysics & Cosmology (United States)
Stanford Univ. (United States)
SLAC National Accelerator Lab. (United States)
A. T. Lee, Univ. of California, Berkeley (United States)
Lawrence Berkeley National Lab. (United States)
E. M. Leitch, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
S. Lendinez, Argonne National Lab. (United States)
S. S. Meyer, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
Enrico Fermi Institute (United States)
C. S. Miller, Argonne National Lab. (United States)
J. Montgomery, McGill Univ. (Canada)
A. Nadolski, Univ. of Illinois at Urbana-Champaign (United States)
T. Natoli, Harvard-Smithsonian Ctr. for Astrophysics (United States)
H. Nguyen, Fermi National Accelerator Lab. (United States)
V. Novosad, Argonne National Lab. (United States)
S. Padin, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
Z. Pan, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
J. Pearson, Argonne National Lab. (United States)
C. M. Posada, Argonne National Lab. (United States)
A. Rahlin, Fermi National Accelerator Lab. (United States)
C. L. Reichardt, The Univ. of Melbourne (Australia)
J. E. Ruhl, Univ. of California, Davis (United States)
B. R. Saliwanchik, Univ. of California, Davis (United States)
J. T. Sayre, Univ. of Colorado at Boulder (United States)
J. A. Shariff, Univ. of California, Davis (United States)
Ian Shirley, Univ. of California, Berkeley (United States)
E. Shirokoff, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
G. Smecher, Case Western Reserve Univ. (United States)
J. Sobrin, Kavli Institute for Cosmological Physics (United States)
The Univ. of Chicago (United States)
L. Stan, Argonne National Lab. (United States)
A. A. Stark, Three-Speed Logic, Inc. (United States)
K. Story, Kavli Institute for Particle Astrophysics & Cosmology (United States)
Stanford Univ. (United States)
A. Suzuki, Univ. of California, Berkeley (United States)
Q. Y. Tang, The Univ. of Chicago (United States)
Kavli Institute for Cosmological Physics (United States)
K. L. Thompson, Kavli Institute for Particle Astrophysics & Cosmology (United States)
Stanford Univ. (United States)
SLAC National Accelerator Lab. (United States)
C. Tucker, Cardiff Univ. (United Kingdom)
K. Vanderlinde, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Univ. of Toronto (Canada)
J. D. Vieira, Univ. of Illinois at Urbana-Champaign (United States)
Dunlap Institute for Astronomy & Astrophysics, Univ. of Toronto (Canada)
G. Wang, Argonne National Lab. (United States)
N. Whitehorn, Univ. of California, Berkeley (United States)
V. Yefremenko, Argonne National Lab. (United States)
K. W. Yoon, Kavli Institute for Particle Astrophysics & Cosmology (United States)
Stanford Univ. (United States)
SLAC National Accelerator Lab. (United States)


Published in SPIE Proceedings Vol. 9914:
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII
Wayne S. Holland; Jonas Zmuidzinas, Editor(s)

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