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International Journal of Infrared and Millimeter Waves

A Fixed-Tuned W-Band Waveguide SIS Mixer with 4.0-7.5 GHz IF

Shin’ichiro Asayama, Takashi Noguchi, Hideo Ogawa

Published Jul 1, 2003• 13 citations
Publisher
DOI
10.1023/a:1024733232384

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Fig. 1. (Top) A 700 GHz finline mixer chip. The finline taper runs from the left to center of the chip, and the mixer tuning circuit, RF block and bond pads are on the right (Bottom) Cross-sections through the finline taper, showing the metallization and the E-field lines. The finline taper gradually transforms the waveguide mode at A through unilateral finline (B) to antipodal finline (C), before transitioning from antipodal finline to microstrip (D-F). Abstract—SIS mixers using finline waveguide to microstrip transitions show a number of advantageous features, particularly in providing a broadband, fixed impedance feed to the SIS mixer tuning circuit. The large chip area and insensitivity to mixer block machining tolerances simplifies the assembly of the mixer, as well as allowing more advanced mixer designs to be fabricated on a single chip. Finline SIS mixers have shown good performance in the 230 and 350 GHz bands[1][2], and we have also previously reported results from two finline SIS mixers in the 600-720 GHz band[3][4], obtaining best receiver noise temperatures of ~250 K. In this paper we present results from several finline mixers in the 600-720 GHz band, using both variants of our original 3-stage Chebyshev filter tuned single junction mixers and new Belitsky tuned mixers. These dual junction tuned mixers show significantly better performance than our previously reported results, with receiver noise temperatures below 200 K. We present detailed SuperMix simulations of the receiver performance and compare these with measured results. We find good agreement between simulations and measured performance can be achieved by introducing a small amount of attenuation in the RF circuit of the mixer. We also present simulations of the IF bandwidth of finline mixers, and suggest a method by which this can be greatly improved.

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We report on the design and characterization of two full height waveguide SIS mixers for astronomical applications: a Double Side Band (DSB) fixed-tuned mixer covering the 225-370 GHz band ( 50 % of relative bandwidth), and a tunable Single Side Band (SSB) mixer covering the 247-360 GHz frequency range. The DSB receiver noise temperature we have measured is below 50 K over a bandwidth larger than 100 GHz for the DSB mixer and has a minimum of 27 K (uncorrected) at 336 GHz; to our knowledge this is the lowest noise ever reported at this frequency. A receiver noise temperature below 80 K and an image band rejection around -14 dB were measured over most of the band of the SSB mixer. Both mixers use similar chips that integrate a parallel tuning inductor with a radial microstrip stub to compensate for the junction capacitance of 75 fF (junction size 1 μm 2 ). A stability criterion for intrinsically DSB and SSB mixers under typical operating conditions has been derived. The receiver designs have been optimised in order to guarantee a low mixer noise temperature while maintaining adequate gain and stable operation over the whole frequency bands of interest.

Journal de Physique IV (Proceedings)•May 1, 2002•5 citations
This paper presents design and performance data for a 100-GHz waveguide superconductor-insulator-superconductor (SIS) mixer, which is incorporated with a twin-junction device (i.e., two identical junctions connected in parallel through a tuning inductance) and a fixed-tuned broad-band waveguide mixer mount. The 100-GHz mixer is actually developed as a prototype of the 500-GHz one. The constructed 100-GHz SIS receiver results in an overall receiver noise temperature (DSB) of less than 40 K over the frequency range from 80-120 GHz, with a minimum value of just 20 K that is four times as large as the quantum limit (i.e., 4/spl planck//spl omega//k). Such a performance is comparable or even superior to those of the best mechanically tunable waveguide SIS receivers at the same frequency band. In addition, some interesting mixing behaviors related to this two-junction device are described in detail.
Fig. 1. (Top) A 700 GHz finline mixer chip. The finline taper runs from the left to center of the chip, and the mixer tuning circuit, RF block and bond pads are on the right (Bottom) Cross-sections through the finline taper, showing the metallization and the E-field lines. The finline taper gradually transforms the waveguide mode at A through unilateral finline (B) to antipodal finline (C), before transitioning from antipodal finline to microstrip (D-F). Abstract—SIS mixers using finline waveguide to microstrip transitions show a number of advantageous features, particularly in providing a broadband, fixed impedance feed to the SIS mixer tuning circuit. The large chip area and insensitivity to mixer block machining tolerances simplifies the assembly of the mixer, as well as allowing more advanced mixer designs to be fabricated on a single chip. Finline SIS mixers have shown good performance in the 230 and 350 GHz bands[1][2], and we have also previously reported results from two finline SIS mixers in the 600-720 GHz band[3][4], obtaining best receiver noise temperatures of ~250 K. In this paper we present results from several finline mixers in the 600-720 GHz band, using both variants of our original 3-stage Chebyshev filter tuned single junction mixers and new Belitsky tuned mixers. These dual junction tuned mixers show significantly better performance than our previously reported results, with receiver noise temperatures below 200 K. We present detailed SuperMix simulations of the receiver performance and compare these with measured results. We find good agreement between simulations and measured performance can be achieved by introducing a small amount of attenuation in the RF circuit of the mixer. We also present simulations of the IF bandwidth of finline mixers, and suggest a method by which this can be greatly improved.
We report on the design and characterization of two full height waveguide SIS mixers for astronomical applications: a Double Side Band (DSB) fixed-tuned mixer covering the 225-370 GHz band ( 50 % of relative bandwidth), and a tunable Single Side Band (SSB) mixer covering the 247-360 GHz frequency range. The DSB receiver noise temperature we have measured is below 50 K over a bandwidth larger than 100 GHz for the DSB mixer and has a minimum of 27 K (uncorrected) at 336 GHz; to our knowledge this is the lowest noise ever reported at this frequency. A receiver noise temperature below 80 K and an image band rejection around -14 dB were measured over most of the band of the SSB mixer. Both mixers use similar chips that integrate a parallel tuning inductor with a radial microstrip stub to compensate for the junction capacitance of 75 fF (junction size 1 μm 2 ). A stability criterion for intrinsically DSB and SSB mixers under typical operating conditions has been derived. The receiver designs have been optimised in order to guarantee a low mixer noise temperature while maintaining adequate gain and stable operation over the whole frequency bands of interest.