A Compact Filter-Bank Waveguide Spectrometer for Millimeter Wavelengths

Bryan, Sean; Che, George; Groppi, Christopher; Mauskopf, Philip Daniel; Underhill, Matthew

doi:10.1109/tthz.2015.2433919

Cited by 12 publications

(12 citation statements)

References 12 publications

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“…This increased length would significantly increase the impact of any waveguide loss on the prototype system. We measured the performance in the lab with the apparatus described in a previous article 10 . A synthesizer generates a single microwave frequency which drives the source port of a WR5 VNA extender.…”

Section: Wr5 Prototype Test Resultsmentioning

confidence: 99%

“…This yields a three-port S-matrix model of each spectrometer channel, which we cascaded together into a complete spectrometer model 10 .…”

Section: Including Detector Effects In the Modelmentioning

confidence: 99%

“…The spectrometer concept is shown in Figure 1, which is a drawing of a prototype WR10 device we built and tested 10 . Broadband light from the sky is coupled into a main waveguide using a feed horn.…”

Section: Introductionmentioning

confidence: 99%

“…Off-resonance, this cancellation does not take place, which keeps out of band radiation from coupling to the detector. The design of a full 54-channel device that fills the single-moded passband of rectangular waveguide is discussed in an earlier publication 10 .…”

Section: Introductionmentioning

confidence: 99%

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WSPEC: A Waveguide Filter-Bank Focal Plane Array Spectrometer for Millimeter Wave Astronomy and Cosmology

Bryan¹,

Aguirre²,

Che³

et al. 2015

J Low Temp Phys

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Imaging and spectroscopy at (sub-)millimeter wavelengths are key frontiers in astronomy and cosmology. Large area spectral surveys with moderate spectral resolution (R=50-200) will be used to characterize large scale structure and star formation through intensity mapping surveys in emission lines such as the CO rotational transitions. Such surveys will also be used to study the SZ effect, and will detect the emission lines and continuum spectrum of individual objects. WSPEC is an instrument proposed to target these science goals. It is a channelizing spectrometer realized in rectangular waveguide, fabricated using conventional high-precision metal machining. Each spectrometer is coupled to free space with a machined feed horn, and the devices are tiled into a 2D array to fill the focal plane of the telescope. The detectors will be aluminum Lumped-Element Kinetic Inductance Detectors (LEKIDs). To target the CO lines and SZ effect, we will have bands at 135-175 GHz and 190-250 GHz, each Nyquist-sampled at R ≈200 resolution. Here we discuss the instrument concept and design, and successful initial testing of a WR10 (i.e. 90 GHz) prototype spectrometer. We recently tested a WR5 (180 GHz) prototype to verify that the concept works at higher frequencies, and also designed a resonant backshort structure that may further increase the optical efficiency. We are making progress towards integrating a spectrometer with a LEKID array and deploying a prototype device to a telescope for first light.

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Section: Wr5 Prototype Test Resultsmentioning

confidence: 99%

“…This yields a three-port S-matrix model of each spectrometer channel, which we cascaded together into a complete spectrometer model 10 .…”

Section: Including Detector Effects In the Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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WSPEC: A Waveguide Filter-Bank Focal Plane Array Spectrometer for Millimeter Wave Astronomy and Cosmology

Bryan¹,

Aguirre²,

Che³

et al. 2015

J Low Temp Phys

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“…To overcome this issue, one feasible solution is to deploy filter bank behind TSAs [56]. Next, phase of a received signal at the output of each filter is changed by using a phase-shifter.…”

Section: Overcoming Small-scale Fadingmentioning

confidence: 99%

mmWave Lens-Based MIMO System for Suppressing Small-Scale Fading and Shadowing

Almasi

Amiri

Jafarkhani

et al. 2020

IEEE Trans. Wireless Commun.

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In this paper, we propose a generalized millimeter-Wave (mmWave) reconfigurable antenna multiple-input multipleoutput (RA-MIMO) architecture that takes advantage of lens antennas. The considered antennas can generate multiple independent beams simultaneously using a single RF chain. This property, together with RA-MIMO, is used to combat smallscale fading and shadowing in mmWave bands. To this end, first, we derive a channel matrix for RA-MIMO. Then, we use rate-one space-time block codes (STBCs), together with phaseshifters at the receive reconfigurable antennas, to suppress the effect of small-scale fading. We consider two kinds of phase shifters: i) ideal which is error-free and ii) digital which adds quantization error. The goal of phase-shifters is to convert a complex-valued channel matrix into real-valued. Hence, it is possible to use rate-one STBCs for any dimension of RA-MIMO. We investigate diversity gain and derive an upper bound for symbol error rate in cases of ideal and digital phase-shifters. We show that RA-MIMO achieves the full-diversity gain with ideal phase-shifters and the full-diversity gain for digital phaseshifters when the number of quantization bits is higher than one. We investigate RA-MIMO in the presence of shadowing. Our analysis demonstrates that, by increasing the dimension of RA-MIMO, the outage probability decreases which means the effect of shadowing decreases. Numerical results verify our theoretical derivations.

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