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Proceedings Paper

SuperSpec: development towards a full-scale filter bank
Author(s): J. Wheeler; S. Hailey-Dunsheath; E. Shirokoff; P. S. Barry; C. M. Bradford; S. Chapman; G. Che; J. Glenn; M. Hollister; A. Kovács; H. G. LeDuc; P. Mauskopf; R. McGeehan; C. M. McKenney; R. O’Brient; S. Padin; T. Reck; C. Ross; C. Shiu; C. E. Tucker; R. Williamson; J. Zmuidzinas
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Paper Abstract

SuperSpec is a new spectrometer-on-a-chip technology for submm/mm-wave spectroscopy. SuperSpec stands out from other direct-detection submm spectrometer technologies in that the detectors are coupled to a series of resonant filters along a single microwave feedline instead of using dispersive optics. SuperSpec makes use of kinetic inductance detectors (KIDs) to detect radiation in this filter bank. The small profile of this design makes SuperSpec a natural choice to produce a multi-object spectrometer for tomographic mapping or galaxy redshift surveys. We have recently fabricated a device that is a 50 channel subset of a full 280 channel filter bank, which would cover the 190 - 310 GHz range at R = 275. Analysis of the data from this device informs us of the potential design modifications to enable a high-yield background-limited SuperSpec spectrometer. The results indicate that this subset filter bank can scale up to a full filter bank with only a few collisions in readout space and less than 20% variation in responsivity for the detectors. Additionally, the characterization of this and other prototype devices suggests that the noise performance is limited by generation-recombination noise. Finally, we find that the detectors are sufficiently sensitive for ground-based spectroscopy at R = 100, appropriate for tomographic mapping experiments. Further modifications are required to reach the background limit for R = 400, ideal for spectroscopy of individual galaxies.

Paper Details

Date Published: 27 July 2016
PDF: 9 pages
Proc. SPIE 9914, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, 99143K (27 July 2016); doi: 10.1117/12.2233798
Show Author Affiliations
J. Wheeler, Univ. of Colorado at Boulder (United States)
S. Hailey-Dunsheath, California Institute of Technology (United States)
E. Shirokoff, The Univ. of Chicago (United States)
P. S. Barry, Cardiff Univ. (United Kingdom)
C. M. Bradford, Jet Propulsion Lab. (United States)
California Institute of Technology (United States)
S. Chapman, Dalhousie Univ. (Canada)
G. Che, Arizona State Univ. (United States)
J. Glenn, Univ. of Colorado at Boulder (United States)
M. Hollister, California Institute of Technology (United States)
A. Kovács, California Institute of Technology (United States)
Univ. of Minnesota (United States)
H. G. LeDuc, Jet Propulsion Lab. (United States)
P. Mauskopf, Arizona State Univ. (United States)
R. McGeehan, Univ. of Chicago (United States)
C. M. McKenney, National Institute of Standards and Technology (United States)
R. O’Brient, Jet Propulsion Lab. (United States)
S. Padin, California Institute of Technology (United States)
T. Reck, Jet Propulsion Lab. (United States)
C. Ross, Dalhousie Univ. (Canada)
C. Shiu, California Institute of Technology (United States)
C. E. Tucker, Cardiff Univ. (United Kingdom)
R. Williamson, Jet Propulsion Lab. (United States)
J. Zmuidzinas, California Institute of Technology (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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