Tuning Circuit Material for Mass-Produced Terahertz SIS Receivers

Uzawa, Yoshinori; Fujii, Yasunori; González, Álvaro; Kaneko, Keiko; Kroug, M.; Kojima, Takafumi; Miyachi, Akihira; Makise, Kazumasa; Saito, Shingo; Terai, Hirotaka; Wang, Z.

doi:10.1109/tasc.2014.2386211

Cited by 24 publications

(24 citation statements)

References 18 publications

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“…Figure 7 demonstrates that all noise performances are compliant with the stringent ALMA specifications. The receivers with all the other SIS mixer chips also met the specifications to complete the delivery of all the receivers to the ALMA project as scheduled (Uzawa et al., 2015). It should be noted that we recently achieved a higher sensitivity and wider bandwidth by implementing our developed Nb/AlNx/Nb junctions with a current density of ∼30 kA/cm 2 (Kroug et al., 2018).…”

Section: Alma Band 10 Receiversmentioning

confidence: 99%

Superconducting Receiver Technologies Supporting ALMA and Future Prospects

et al. 2021

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The Atacama Large Millimeter/submillimeter Array (ALMA) is the most sensitive ground-based radio astronomical telescope (see Figure 1) (ALMA observatory; URL: http://www.almaobservatory.org). Located in the Atacama Desert, 5,000 m above sea level in northern Chile, South America, it is a collaboration between East Asia, Europe, and North America. ALMA consists of fifty-four 12-m-diameter antennas and twelve 7-m-diameter antennas. The observation frequencies range from 35 GHz (millimeter waves) to 950 GHz (submillimeter waves). With such radio frequency (RF) observations, it is possible to capture the amplitudes and phases of signals from astronomical objects and by performing a proper interference of those signals, a single large synthesized radio telescope can be formed. This method is called aperture synthesis and was developed by radio astronomer Martin Ryle at Cambridge University (Ryle, 1975), for which he was awarded the Nobel Prize in Physics in 1974. The spatial angular resolution is determined by the antenna array configuration and observation frequency. The distance between ALMA antennas can be extended up to 16 km, allowing a maximum angular resolution of less than 0.01″, which is why the term "large" is used in the name. The achievable angular resolution of ALMA is 10 times higher than those of the Subaru Telescope and Hubble Space Telescope and up to 100 times higher than those of the existing millimeter/submillimeter telescopes.ALMA also offers unpreceded sensitivity. Owing to its large collecting area of over 6,600 m 2 and highly sensitive receivers using superconductor-insulator-superconductor (SIS) mixers along with high-electron-mobility transistor (HEMT) amplifiers, ALMA has a sensitivity 2 orders of magnitude better than those of the existing radio telescopes. Most of the SIS mixers in ALMA utilize superconducting niobium (Nb)

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Section: Alma Band 10 Receiversmentioning

confidence: 99%

Superconducting Receiver Technologies Supporting ALMA and Future Prospects

et al. 2021

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“…SIS mixer tuning circuits above this frequency use a combination of higher gap superconducting materials like NbTiN and normal conducting metals like gold or aluminum [60,61]. Up to 700 GHz SIS mixers reach quantum limited sensitivity.…”

Section: Superconductor-insulator-superconductor Devicesmentioning

confidence: 99%

Terahertz Heterodyne Array Receivers for Astronomy

Graf

Honingh

Jacobs

et al. 2015

J Infrared Milli Terahz Waves

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We review the development of multi-pixel heterodyne receivers for astronomical research in the submillimeter and terahertz spectral domains. We shortly address the historical development, highlighting a few pioneering instruments. A discussion of the design concepts is followed by a presentation of the technologies employed in the various receiver subsystems and of the approaches taken to optimize these for current and future instruments.

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“…However, it is in principle difficult to achieve IF bandwidths greater than 10 GHz because the mixing mechanism is fundamentally limited (Novoselov & Cherednichenko 2017). On the other hand, receivers based on superconductor-insulatorsuperconductor (SIS) mixers at submillimeter wavelengths, up to about 1 THz, have attained quantum-limited low-noise performance with an RF fractional bandwidth of 20-30%, and IF 4-8 GHz (Billade et al 2013;Kerr & Pan 2014;Mahieu et al 2012;Tamura et al 2015), or 4-12 GHz (Baryshev et al 2015;Uzawa et al 2015). In recent years, several studies have attempted to increase the RF (Kojima et al 2017) and IF (Tong 2015;Kojima et al 2018) bandwidth of SIS mixers independently.…”

Section: Introductionmentioning

confidence: 99%

Demonstration of a wideband submillimeter-wave low-noise receiver with 4–21 GHz IF output digitized by a high-speed 32 GSps ADC

Kojima

Kiuchi

Uemizu

et al. 2020

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We report on a 275–500 GHz heterodyne receiver system in combination with a wideband intermediate-frequency (IF) backend to realize 17 GHz instantaneous bandwidth. The receiver frontend implements a heterodyne mixer module that integrates a superconductor-insulator-superconductor (SIS) mixer chip and a cryogenic low-noise preamplifier. The SIS mixer is developed based on high-current-density junction technologies to achieve a wideband radio frequency (RF) and IF bandwidth. The IF backend comprises an IF chain divided into two channels for 4.0–11.5 GHz and 11.3–21.0 GHz and an analog-to-digital converter (ADC) module that is capable of high-speed sampling at 32 Giga samples per second with 12.5 GHz bandwidth per channel and an effective number of bits of 6.5. The IF backend allows us to simultaneously cover the full 4–21 GHz IF range of the receiver frontend. The measured noise temperature of the receiver frontend was below three times the quantum noise (hf/kB) over the entire RF band. A dual-polarization sideband-separating receiver based on this technique could provide up to 64 GHz of instantaneous bandwidth, which demonstrates the possibility of future wideband radio astronomical observations with advanced submillimeter-wave heterodyne receivers.

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Tuning Circuit Material for Mass-Produced Terahertz SIS Receivers

Cited by 24 publications

References 18 publications

Superconducting Receiver Technologies Supporting ALMA and Future Prospects

Superconducting Receiver Technologies Supporting ALMA and Future Prospects

Terahertz Heterodyne Array Receivers for Astronomy

Demonstration of a wideband submillimeter-wave low-noise receiver with 4–21 GHz IF output digitized by a high-speed 32 GSps ADC

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