| Records |
| Author |
Shitov, S. V.; Levitchev, M.; Veretennikov, A. V.; Koshelets, V. P.; Prokopenko, G. V.; Filippenko, L. V.; Ermakov, A. B.; Shtanyuk, A. M.; Kohlstedt, H.; Ustinov, A. V. |
| Title |
Superconducting integrated receiver as 400-600 GHz tester for coolable devices |
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Journal Article |
| Year |
2001 |
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IEEE Trans. Appl. Supercond. |
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11 |
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1 |
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832-835 |
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RPLAB @ s @ sis_Shitov_2001 |
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313 |
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Jackson, B. D.; Baryshev, A. M.; de Lange, G.; Gao, J. R.; Shitov, S. V.; Iosad, N. N.; Klapwijk, T. M. |
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Low-noise 1 THz superconductor-insulator-superconductor mixer incorporating a NbTiN/SiO2/Al tuning circuit |
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Journal Article |
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2001 |
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Appl. Phys. Lett. |
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79 |
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3 |
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436 |
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RPLAB @ s @ sis_Jackson_2001 |
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314 |
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Koshelets, V. P.; Shitov, S. V.; Dmitriev, P. N., Ermakov, A. B.; Filippenko, L. V.; Koryukin, O.V.; Sobolev, A.S.; Torgashin, M.Yu.; Yagoubov, P.; Hoogeveen, R. |
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Integrated submillimeter and terahertz receivers with superconducting local oscillator |
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2004 |
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Presanted at 8th International Workshop “From Andreev Reflection to the International Space Station” |
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513 |
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Shitov, S. V.; Inatani, J.; Shan, W.-L.; Takeda, M; Wang, Z.; Uvarov, A. V.; Ermakov, A. B.; Uzawa, Y. |
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Measurement of emissivity of the ALMA antenna panel at 840 GHz using NbN-based heterodyne SIS receiver |
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Conference Article |
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2008 |
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Proc. 19th Int. Symp. Space Terahertz Technol. |
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263-266 |
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SIS mixer, reflection, emissivity, mirror, space telescope, space observatory |
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580 |
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Uzawa, Y.; Kojima, T.; Kroug, M.; Takeda, M.; Candotti, M.; Fujii, Y.; Shan, W.-L.; Kaneko, K.; Shitov, S.; Wang, M.-J. |
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Development of the 787-950 GHz ALMA band 10 cartridge |
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Conference Article |
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2009 |
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Proc. 20th Int. Symp. Space Terahertz Technol. |
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12-12 |
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SIS mixer, noise temperature, ALMA, band 10 |
| Abstract |
We are developing the Atacama Large Millimeter/Submillimeter Array (ALMA) Band 10 (787-950 GHz) receiver cartridge. The incoming beam from the 12-m antenna is reflected by a pair of two ellipsoidal mirrors placed in the cartridge, and then split into two orthogonal polarizations by a free-standing wire-grid. Each beam enters a corrugated feed horn attached to a double-side-band (DSB) mixer block. The mixer uses a full-height waveguide and an NbTiN- or NbN-based superconductor-insulator-superconductor (SIS) mixer chip. We are testing the following three types of mixer chips: 1) Nb SIS junctions + NbTiN/SiO2/Al tuning circuits on a quartz substrate, 2) Nb SIS junctions + NbN/SiO2/Al tuning circuits on an MgO substrate, and 3) NbN SIS junctions + NbN or NbTiN tuning circuits on an MgO substrate. The IF system uses a 4-12-GHz cooled low-noise InP-based MMIC amplifier developed by Caltech. So far, the type 1) has shown the best performance. At LO frequencies from 800 to 940 GHz, the mixer noise temperatures measured by using the standard Y-factor method were below 240 K at an operating physical temperature of 4 K. The lowest noise temperature, 169 K, was obtained at the center frequency of the band 10, as designed. These well-developed technologies will be implemented in the band 10 cartridge to achieve the ALMA specifications. |
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615 |
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