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Proceedings Paper

MKID development for SuperSpec: an on-chip, mm-wave, filter-bank spectrometer
Author(s): E. Shirokoff; P. S. Barry; C. M. Bradford; G. Chattopadhyay; P. Day; S. Doyle; S. Hailey-Dunsheath; M. I. Hollister; A. Kovács; C. McKenney; H. G. Leduc; N. Llombart; D. P. Marrone; P. Mauskopf; R. O'Brient; S. Padin; T. Reck; L. J. Swenson; J. Zmuidzinas
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Paper Abstract

SuperSpec is an ultra-compact spectrometer-on-a-chip for millimeter and submillimeter wavelength astronomy. Its very small size, wide spectral bandwidth, and highly multiplexed readout will enable construction of powerful multibeam spectrometers for high-redshift observations. The spectrometer consists of a horn-coupled microstrip feedline, a bank of narrow-band superconducting resonator filters that provide spectral selectivity, and kinetic inductance detectors (KIDs) that detect the power admitted by each filter resonator. The design is realized using thin-film lithographic structures on a silicon wafer. The mm-wave microstrip feedline and spectral filters of the first prototype are designed to operate in the band from 195-310 GHz and are fabricated from niobium with at Tc of 9.2K. The KIDs are designed to operate at hundreds of MHz and are fabricated from titanium nitride with a Tc of ~ 2 K. Radiation incident on the horn travels along the mm-wave microstrip, passes through the frequency-selective filter, and is finally absorbed by the corresponding KID where it causes a measurable shift in the resonant frequency. In this proceedings, we present the design of the KIDs employed in SuperSpec and the results of initial laboratory testing of a prototype device. We will also brie describe the ongoing development of a demonstration instrument that will consist of two 500-channel, R=700 spectrometers, one operating in the 1-mm atmospheric window and the other covering the 650 and 850 micron bands.

Paper Details

Date Published: 27 September 2012
PDF: 11 pages
Proc. SPIE 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 84520R (27 September 2012); doi: 10.1117/12.927070
Show Author Affiliations
E. Shirokoff, California Institute of Technology (United States)
P. S. Barry, Cardiff Univ. (United Kingdom)
C. M. Bradford, Jet Propulsion Lab. (United States)
G. Chattopadhyay, Jet Propulsion Lab. (United States)
P. Day, Jet Propulsion Lab. (United States)
S. Doyle, Cardiff Univ. (United Kingdom)
S. Hailey-Dunsheath, California Institute of Technology (United States)
M. I. Hollister, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)
A. Kovács, California Institute of Technology (United States)
Univ. of Minnesota, Twin Cities (United States)
C. McKenney, California Institute of Technology (United States)
H. G. Leduc, Jet Propulsion Lab. (United States)
N. Llombart, Complutense Univ. of Madrid (Spain)
D. P. Marrone, The Univ. of Arizona (United States)
P. Mauskopf, Cardiff Univ. (United Kingdom)
Arizona State Univ. (United States)
R. O'Brient, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)
S. Padin, California Institute of Technology (United States)
T. Reck, Jet Propulsion Lab. (United States)
L. J. Swenson, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)
J. Zmuidzinas, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)


Published in SPIE Proceedings Vol. 8452:
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI
Wayne S. Holland, Editor(s)

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