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Proceedings Paper

Design of 280 GHz feedhorn-coupled TES arrays for the balloon-borne polarimeter SPIDER
Author(s): Johannes Hubmayr; Jason E. Austermann; James A. Beall; Daniel T. Becker; Steven J. Benton; A. Stevie Bergman; J. Richard Bond; Sean Bryan; Shannon M. Duff; Adri J. Duivenvoorden; H. K. Eriksen; Jeffrey P. Filippini; A. Fraisse; Mathew Galloway; Anne E. Gambrel; K. Ganga; Arpi L. Grigorian; Riccardo Gualtieri; Jon E. Gudmundsson; John W. Hartley; M. Halpern; Gene C. Hilton; William C. Jones; Jeffrey J. McMahon; Lorenzo Moncelsi; Johanna M. Nagy; C. B. Netterfield; Benjamin Osherson; Ivan Padilla; Alexandra S. Rahlin; B. Racine; John Ruhl; T. M. Rudd; J. A. Shariff; J. D. Soler; Xue Song; Joel N. Ullom; Jeff Van Lanen; Michael R. Vissers; I. K. Wehus; Shyang Wen; D. V. Wiebe; Edward Young
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Paper Abstract

We describe 280 GHz bolometric detector arrays that instrument the balloon-borne polarimeter spider. A primary science goal of spider is to measure the large-scale B-mode polarization of the cosmic microwave background (cmb) in search of the cosmic-inflation, gravitational-wave signature. 280 GHz channels aid this science goal by constraining the level of B-mode contamination from galactic dust emission. We present the focal plane unit design, which consists of a 16x16 array of conical, corrugated feedhorns coupled to a monolithic detector array fabricated on a 150 mm diameter silicon wafer. Detector arrays are capable of polarimetric sensing via waveguide probe-coupling to a multiplexed array of transition-edge-sensor (TES) bolometers. The spider receiver has three focal plane units at 280 GHz, which in total contains 765 spatial pixels and 1,530 polarization sensitive bolometers. By fabrication and measurement of single feedhorns, we demonstrate 14.7° FHWM Gaussian-shaped beams with <1% ellipticity in a 30% fractional bandwidth centered at 280 GHz. We present electromagnetic simulations of the detection circuit, which show 94% band-averaged, single-polarization coupling efficiency, 3% reflection and 3% radiative loss. Lastly, we demonstrate a low thermal conductance bolometer, which is well-described by a simple TES model and exhibits an electrical noise equivalent power (NEP) = 2.6 x 10-17 W/√Hz, consistent with the phonon noise prediction.

Paper Details

Date Published: 19 July 2016
PDF: 14 pages
Proc. SPIE 9914, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, 99140V (19 July 2016); doi: 10.1117/12.2231896
Show Author Affiliations
Johannes Hubmayr, National Institute of Standards and Technology (United States)
Jason E. Austermann, National Institute of Standards and Technology (United States)
James A. Beall, National Institute of Standards and Technology (United States)
Daniel T. Becker, National Institute of Standards and Technology (United States)
Steven J. Benton, Princeton Univ. (United States)
A. Stevie Bergman, Princeton Univ. (United States)
J. Richard Bond, Canadian Institute for Theoretical Astrophysics, Univ. of Toronto (Canada)
Sean Bryan, Arizona State Univ. (United States)
Shannon M. Duff, National Institute of Standards and Technology (United States)
Adri J. Duivenvoorden, Stockholm Univ. (Sweden)
H. K. Eriksen, Univ. of Oslo (Norway)
Jeffrey P. Filippini, Univ. of Illinois at Urbana-Champaign (United States)
A. Fraisse, Princeton Univ. (United States)
Mathew Galloway, Univ. of Toronto (Canada)
Anne E. Gambrel, Princeton Univ. (United States)
K. Ganga, AstroParticule et Cosmologie, Univ. of Paris-Diderot (France)
Arpi L. Grigorian, National Institute of Standards and Technology (United States)
Riccardo Gualtieri, Univ. of Illinois at Urbana-Champaign (United States)
Jon E. Gudmundsson, Princeton Univ. (United States)
John W. Hartley, Univ. of Toronto (Canada)
M. Halpern, The Univ. of British Columbia (Canada)
Gene C. Hilton, National Institute of Standards and Technology (United States)
William C. Jones, Princeton Univ. (United States)
Jeffrey J. McMahon, Univ. of Michigan (United States)
Lorenzo Moncelsi, California Institute of Technology (United States)
Johanna M. Nagy, Case Western Reserve Univ. (United States)
C. B. Netterfield, Univ. of Toronto (Canada)
Benjamin Osherson, Univ. of Illinois at Urbana-Champaign (United States)
Ivan Padilla, Univ. of Toronto (Canada)
Alexandra S. Rahlin, Princeton Univ. (United States)
B. Racine, Univ. of Oslo (Norway)
John Ruhl, Case Western Reserve Univ. (United States)
T. M. Rudd, Univ. of Oslo (Norway)
J. A. Shariff, Case Western Reserve Univ. (United States)
J. D. Soler, Lab. AIM, Paris-Saclay, Univ. Paris Diderot (France)
Xue Song, Princeton Univ. (United States)
Joel N. Ullom, National Institute of Standards and Technology (United States)
Jeff Van Lanen, National Institute of Standards and Technology (United States)
Michael R. Vissers, National Institute of Standards and Technology (United States)
I. K. Wehus, Univ. of Oslo (Norway)
Shyang Wen, Case Western Reserve Univ. (United States)
D. V. Wiebe, The Univ. of British Columbia (Canada)
Edward Young, Princeton Univ. (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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