275–500-GHz Wideband Waveguide SIS Mixers

Kojima, Takafumi; Kroug, M.; González, Álvaro; Uemizu, Kazunori; Kaneko, Keiko; Miyachi, Akihira; Kozuki, Yuto; Asayama, Shin’ichiro

doi:10.1109/tthz.2018.2873487

Cited by 18 publications

(14 citation statements)

References 14 publications

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“…The SIS-mixer-preamplifier module used in this study is composed of four parts: (1) the main metal body, which provides support for the other parts and a WR-2.3 waveguide interface for the RF signal input, (2) a superconducting magnetic coil, (3) a dropin-type CLNA with a 4-21 GHz IF output, and (4) the SIS mixer chip. The basic design concepts of the RF and IF circuitries are similar to the design previously described in Kojima et al (2018) and Kojima et al (2017), respectively, while the IF-matching circuit in the SIS mixer chip is optimized to maximize the IF bandwidth of the module. The SIS mixer chip is mounted onto the mixer chip slot inside the main body, and is directly connected with the CLNA by bonding wires.…”

Section: Discussionmentioning

confidence: 99%

“…In the cryostat, a wideband corrugated horn antenna, a WR-2.3 waveguide LO/RF coupler with a coupling ratio of around 15 dB, and the SIS-mixer-preamplifier module are placed on the 4-K stage. The design and performance of the RF components are described in previous papers (Gonzalez et al 2017a;Kojima et al 2018). The key component in the receiver frontend is a low-noise heterodyne mixer module to achieve wide RF and IF coverage.…”

Section: Receiver Systemmentioning

confidence: 99%

“…The CLNA, manufactured by Low Noise Factory 2 , has a typical gain and noise temperature of 35 dB and 5 K over 3-22 GHz. It incorporates an input-matching circuit optimized for 50Ω standard impedance and a bias-tee circuit for the SIS junctions (Kojima et al 2018).…”

Section: Receiver Systemmentioning

confidence: 99%

“…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. This work has proven very challenging in terms of maintaining current advanced noise-temperature performance because there are some fundamental trade-offs in terms of bandwidth and Full receiver system developed in this study.…”

Section: Introductionmentioning

confidence: 99%

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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

A&A

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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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Section: Discussionmentioning

confidence: 99%

Section: Receiver Systemmentioning

confidence: 99%

Section: Receiver Systemmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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

A&A

Self Cite

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“…To our knowledge, this is the widest submillimeter-wave mixer with quantumlimited performance in terms of RF and IF. The basic design concepts of the RF and IF circuitries are similar to those previously described in [52] and [53], respectively, while the IF-matching circuit in the SIS mixer chip is optimized to maximize the IF bandwidth of the module. Figure 7 shows the design of the wideband RF and IF SIS mixer chip.…”

Section: Sis Mixer Device Developmentmentioning

confidence: 99%

Development of Superconducting Devices Supporting Radio Astronomy

Uzawa¹,

Kroug

Kojima³

et al. 2021

IEICE Trans. Electron.

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This paper describes the development of superconductorinsulator-superconductor (SIS) mixers for the Atacama Large Millimeter/submillimeter Array (ALMA) from the device point of view. During the construction phase of ALMA, the National Astronomical Observatory of Japan (NAOJ) successfully fabricated SIS mixers to meet the stringent ALMA noise temperature requirements of less than 230 K (5 times the quantum noise) for Band 10 (787-950 GHz) in collaboration with the National Institute of Information and Communications Technology. Band 10 covers the highest frequency band of ALMA and is recognized as the most difficult band in terms of superconducting technology. After the construction, the NAOJ began development studies for ALMA enhancement such as wideband and multibeam SIS mixers according to top-level science requirements, which are also presented.

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