NbN hot electron bolometric mixers-a new technology for low noise THz receivers

Gerecht, Eyal; Musante, C.; Zhuang, Yan; Goyette, Thomas M.; Dickinson, Jason C.; Waldman, J.; Yagoubov, P.; Gol’tsman, G.; Voronov, B.; Gershenzon, E.

doi:10.1109/mwsym.1999.780319

Cited by 19 publications

(12 citation statements)

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“…Parylene C coatings were used to substantially increase the transmittance of the optics with transmission peaks approaching 90%. Another device which would benefit significantly from low-loss AR coatings at terahertz frequencies is the superconducting hot-electron bolometer (HEB) [5]. These sensitive detectors of terahertz radiation typically use small silicon lenses to focus radiation onto an antenna-coupled detector element.…”

Section: Introductionmentioning

confidence: 99%

An anti-reflection coating for silicon optics at terahertz frequencies

Gatesman

Waldman

et al. 2000

IEEE Microw. Guid. Wave Lett.

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140

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A method for reducing the reflections from silicon optics at terahertz frequencies has been investigated. In this study, we used thin films of parylene as an anti-reflection (AR) layer for silicon optics and show low-loss behavior well above 1 THz. Transmittance spectra are acquired on double-sided-parylene-coated, high-resistivity, single-crystal silicon etalons between 0.45 THz and 2.8 THz. Modeling the optical behavior of the three-layer system allowed for the determination of the refractive index and absorption coefficient of parylene at these frequencies. Our data indicate a refractive index, , of 1.62 for parylene C and parylene D, and a reasonably modest absorption coefficient make these materials a suitable AR coating for silicon at terahertz frequencies. Coatings sufficiently thick for AR performance reduced the average transmittance of the three-layer system by 10% compared to a lossless AR coating with an ideal refractive index.

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Section: Introductionmentioning

confidence: 99%

An anti-reflection coating for silicon optics at terahertz frequencies

Gatesman

Waldman

et al. 2000

IEEE Microw. Guid. Wave Lett.

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140

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“…Two Terahertz detector systems were installed on AST/RO as guest instruments: the Terahertz Receiver with NbN HEB Device (TREND) was a heterodyne receiver with a LASER local oscillator (Gerecht et al 1999, Yngvesson et al 2002; and the South Pole Imaging Fabry-Perot Interferometer (SPIFI, Swain et al 1998, Bradford et al 2002. The principal difficulty in Terahertz operation was that when engineering teams could be brought in during the Austral summer, the sky was not transparent enough even for testing, so an untried system would be left for the winterover scientists to attempt first light during brief winter periods of marginal Terahertz weather.…”

Section: Science Resultsmentioning

confidence: 99%

Submillimeter Astronomy from the South Pole (AST/RO)

Stark

2012

Proc. IAU

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Abstract. The Antarctic Submillimeter Telescope and Remote Observatory (AST/RO), a 1.7 m diameter offset Gregorian telescope for astronomy and aeronomy studies at wavelengths between 200 and 2000 μm, saw first light in 1995 and operated until 2005. It was the first radio telescope to operate continuously throughout the winter on the Antarctic Plateau. It served as a site testing instrument and prototype for later instruments, as well as executing a wide variety of scientific programs that resulted in six doctoral theses and more than one hundred scientific publications. The South Pole environment is unique among observatory sites for unusually low wind speeds, low absolute humidity, and the consistent clarity of the submillimeter sky. Especially significant are the exceptionally low values of sky noise found at this site, a result of the small water vapor content of the atmosphere. Multiple submillimeter-wave and Terahertz detector systems were in operation on AST/RO, including heterodyne and bolometric arrays. AST/RO's legacy includes comprehensive submillimeter-wave site testing of the South Pole, spectroscopic studies of 492 GHz and 809 GHz neutral atomic carbon and 460 GHz and 806 GHz carbon monoxide in the Milky Way and Magellanic Clouds, and the first detection of the 1.46 THz [N II] line from a ground-based observatory.

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“…It was used primarily for spectroscopic studies of neutral atomic carbon and carbon monoxide in the interstellar medium of the Milky Way and the Magellanic Clouds. Six heterodyne receivers and a bolometer array were used on AST/RO: (1) a 230 GHz receiver (Kooi et al, 1992), ( 2) a 450-495 GHz quasioptical receiver (Zmuidzinas and LeDuc, 1992;Engargiola et al, 1994), ( 3) a 450-495 GHz waveguide receiver (Walker et al, 1992;Kooi et al, 1995), which could be used simultaneously with ( 4) a 800-820 GHz fixed-tuned superconductor-insulator-superconductor (SIS) waveguide mixer receiver (Honingh et al, 1997), (5) the PoleSTAR array, which deployed four 810 GHz fixed-tuned SIS waveguide mixer receivers (Groppi et al, 2000;Walker et al, 2001), ( 6) Terahertz Receiver with NbN HEB Device (TREND), a 1.5 THz heterodyne receiver (Gerecht et al, 1999;Yngvesson et al, 2001), and ( 7) the South Pole Imaging Fabry-Perot Interferometer (SPIFI; Swain et al, 1998). There were four acousto-optical spectrometers (AOS; Schieder et al, 1989): two low-resolution spectrometers with a bandwidth of 1 GHz, an array AOS having four low-resolution spectrometer channels with a bandwidth of 1 GHz for the PoleSTAR array, and one highresolution AOS with 60 MHz bandwidth.…”

Section: Telescopes and Instruments At The South Polementioning

confidence: 99%

Science Diplomacy: Antarctica, Science, and the Governance of International Spaces

Brady

2011

The Polar Journal

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Finally, such a complex meeting could not have been executed so smoothly without professional assistance of the highest order, and we thank Linder & Associates for their excellent event management, which was contributed with creative enthusiasm. Importantly, as editors, we are grateful to the many reviewers who provided thoughtful assessments of the papers in this volume.The Agreed Measures for the Conservation of Antarctic Fauna and Flora (AMCAFF), adopted by the Consultative Parties at Antarctic Treaty Consultative Meeting (ATCM) III (1964), was the first more-ambitious attempt to adopt elaborate conservation measures for Antarctica. The potential need for measures with respect to the preservation and conservation of living resources in Antarctica was foreseen in the Antarctic Treaty. The First Consultative Meeting had already addressed the issue in Recommendation I-VIII, and it could be said that AMCAFF grew out of that recommendation. The Agreed Measures for the Conservation of Antarctic Fauna and Flora was not labelled a convention, but its form indirectly indicates its status as a treaty under the Antarctic Treaty. The Agreed Measures for the Conservation of Antarctic Fauna and Flora is considered by the Treaty Parties and by some authors as a comprehensive successful international instrument for wildlife conservation. It foreshadows a development within the treaty system with respect to environmental protection, transparency, information sharing, and the role of international organisations, namely, the Scientific Committee on Antarctic Research (SCAR).

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NbN hot electron bolometric mixers-a new technology for low noise THz receivers

Cited by 19 publications

References 9 publications

An anti-reflection coating for silicon optics at terahertz frequencies

An anti-reflection coating for silicon optics at terahertz frequencies

Submillimeter Astronomy from the South Pole (AST/RO)

Science Diplomacy: Antarctica, Science, and the Governance of International Spaces

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