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Proceedings Paper

Automated SQUID tuning procedure for kilo-pixel arrays of TES bolometers on the Atacama Cosmology Telescope
Author(s): E. S. Battistelli; M. Amiri; B. Burger; M. J. Devlin; S. R. Dicker; W. B. Doriese; R. Dünner; R. P. Fisher; J. W. Fowler; M. Halpern; M. Hasselfield; G. C. Hilton; A. D. Hincks; K. D. Irwin; M. Kaul; J. Klein; S. Knotek; J. M. Lau; M. Limon; T. A. Marriage; M. D. Niemack; L. Page; C. D. Reintsema; S. T. Staggs; D. S. Swetz; E. R. Switzer; R. J. Thornton; Y. Zhao
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Paper Abstract

The Atacama Cosmology Telescope observes the Cosmic Microwave Background with arcminute resolution from the Atacama desert in Chile. For the first observing season one array of 32 x 32 Transition Edge Sensor (TES) bolometers was installed in the primary ACT receiver, the Millimeter Bolometer Array Camera (MBAC). In the next season, three independent arrays working at 145, 220 and 280 GHz will be installed in MBAC. The three bolometer arrays are each coupled to a time-domain multiplexer developed at the National Institute of Standard and Technology, Boulder, which comprises three stages of superconducting quantum interference devices (SQUIDs). The arrays and multiplexers are read-out and controlled by the Multi Channel Electronics (MCE) developed at the University of British Columbia, Vancouver. A number of experiments plan to use the MCE as read-out electronics and thus the procedure for tuning the three stage SQUID system is of general interest. Here we describe the automated array tuning procedures and algorithms we have developed. During array tuning, the SQUIDs are biased near their critical currents. SQUID feedback currents and lock points are selected to maximize linearity, dynamic range, and gain of the SQUID response curves. Our automatic array characterization optimizes the tuning of all three stages of SQUIDs by selecting over 1100 parameters per array during the first observing season and over 2100 parameters during the second observing season. We discuss the timing, performance, and reliability of this array tuning procedure as well as planned and recently implemented improvements.

Paper Details

Date Published: 18 July 2008
PDF: 12 pages
Proc. SPIE 7020, Millimeter and Submillimeter Detectors and Instrumentation for Astronomy IV, 702028 (18 July 2008); doi: 10.1117/12.789738
Show Author Affiliations
E. S. Battistelli, Univ. of British Columbia (Canada)
Univ. of Rome La Sapienza (Italy)
M. Amiri, Univ. of British Columbia (Canada)
B. Burger, Univ. of British Columbia (Canada)
M. J. Devlin, Univ. of Pennsylvania (United States)
S. R. Dicker, Univ. of Pennsylvania (United States)
W. B. Doriese, National Institute of Standards and Technology (United States)
R. Dünner, Pontificia Univ. Católica de Chile (Chile)
R. P. Fisher, Princeton Univ. (United States)
J. W. Fowler, Princeton Univ. (United States)
M. Halpern, Univ. of British Columbia (Canada)
M. Hasselfield, Univ. of British Columbia (Canada)
G. C. Hilton, National Institute of Standards and Technology (United States)
A. D. Hincks, Princeton Univ. (United States)
K. D. Irwin, National Institute of Standards and Technology (United States)
M. Kaul, Univ. of Pennsylvania (United States)
J. Klein, Univ. of Pennsylvania (United States)
S. Knotek, Univ. of British Columbia (Canada)
J. M. Lau, Stanford Univ. (United States)
M. Limon, Columbia Astrophysics Lab. (United States)
T. A. Marriage, Princeton Univ. (United States)
M. D. Niemack, Princeton Univ. (United States)
L. Page, Princeton Univ. (United States)
C. D. Reintsema, National Institute of Standards and Technology (United States)
S. T. Staggs, Princeton Univ. (United States)
D. S. Swetz, Univ. of Pennsylvania (United States)
E. R. Switzer, Princeton Univ. (United States)
R. J. Thornton, Univ. of Pennsylvania (United States)
Y. Zhao, Princeton Univ. (United States)

Published in SPIE Proceedings Vol. 7020:
Millimeter and Submillimeter Detectors and Instrumentation for Astronomy IV
William D. Duncan; Wayne S. Holland; Stafford Withington; Jonas Zmuidzinas, Editor(s)

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