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Wengler, M. J. (1992). Submillimeter-wave detection with superconducting tunnel diodes. In Proc. IEEE (Vol. 80, pp. 1810–1826).
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Phillips, T. G., & Keene, J. (1992). Submillimeter astronomy [heterodyne spectroscopy]. In Proc. IEEE (Vol. 80, pp. 1662–1678).
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Gershenzon, E. M., Gol'tsman, G. N., Semenov, A. D., & Sergeev, A. V. (1992). Heating of electrons in resistive state of superconducting films. Detectors, mixers and switches. In Progress in High Temperature Superconductivity (Vol. 32, pp. 190–195).
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Kollberg, E. L., Gershenzon, E., Goltsman, G., & Yngvesson, K. S. (1992). Hot electron mixers, the potential competition. In Proc. ESA Symp. on Photon Detectors for Space Instrumentation (pp. 201–206).
Abstract: There is an urgent need in radio astronomy for low noise heterodyne receivers for frequencies above about 500 GHz. It is not certain that mixers based on superconducting quasiparticle tunnelling (SIS mixers) may turn out to be the answer to this need. In order to try to find an alternative way for realizing low noise heterodyne receivers for submillimeter waves, so called hot electron bolometric effects for mixing are now being investigated. Two basically different approaches are tried, one based on semiconductors and one on superconductors. Both methods are briefly discussed in this overview paper.
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Nebosis, R. S., Steinke, R., Lang, P. T., Schatz, W., Heusinger, M. A., Renk, K. F., et al. (1992). Picosecond YBa2Cu3O7−δdetector for far‐infrared radiation. J. Appl. Phys., 72(11), 5496–5499.
Abstract: We report on a picosecond YBa2Cu3O7−δ detector for far‐infrared radiation. The detector, consisting of a current carrying structure cooled to liquid‐nitrogen temperature, was studied by use of ultrashort laser pulses from an optically pumped far‐infrared laser in the frequency range from 25 to 215 cm−1. We found that the sensitivity (1 mV/W) was almost constant in this frequency range. We estimated a noise equivalent power of less than 5×10−7 W Hz−1/2. Taking into account the results of a mixing experiment (in the frequency range from 4 to 30 cm−1) we suggest that the response time of the detector was few picoseconds.
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