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Елезов, М. С., Корнеев, А. А., Дивочий, А. В., & Гольцман, Г. Н. (2009). Сверхпроводящие однофотонные детекторы с разрешением числа фотонов. In Науч. сессия МИФИ (pp. 47–58).
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Флоря, И. Н. (2009). Ультрабыстрый однофотонный детектор для оптических применений. In Науч. сессия МИФИ (pp. 45–46).
Abstract: Представлен сверхпроводниковый однофотонный детектор (SSPD) на основе ультратонкой пленки NbN, обладающий рекордным быстродействием. Активный элемент выполнен в виде N сверхпроводящих полосок соединенных параллельно, покрывающих площадку размером 10 мкм х 10 мкм. Для SSPD с N=12 длительность импульса напряжения составляет 200 пс. Полученные результаты открывают путь к детекторам обладающими скоростью счета свыше 1 ГГц, что делает SSPDs весьма привлекательными во многих применениях, в частности для квантовой криптографии. SSPD хорошо согласуется с оптоволокном и легко может быть интегрирован в полностью готовую для работы приемную систему.
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Ozhegov, R. V., Smirnov, A. V., Vakhtomin, Y. B., Smirnov, K. V., Divochiy, A. V., & Goltsman, G. N. (2009). Ultrafast superconducting bolometer receivers for terahertz applications. In Proc. PIERS (867). 777 Concord Avenue, Suite 207 Cambridge, MA 02138: The Electromagnetics Academy.
Abstract: The research by the group of Moscow State Pedagogical University into the hot-electron phenomena in thin superconducting films has led to the development of new types of detectors and their use both in fundamental and applied studies. In this paper, we present the results of testing the terahertz HEB receiver systems based on ultrathin (∼ 4 nm) NbN and MoRe detectors with a response time of 50 ps and 1 ns, respectively. We have developed three types of devices which differ in the way a terahertz signal is coupled to the detector and cover the following ranges: 0.3–3 THz, 0.1–30 THz and 25–70 THz. In the case of the receiving system optimized for 0.3–3 THz, the sensitive element (a strip of asuperconductor with planar dimensions of 0.2μm (length) by 1.7μm (width)) was integrated witha planar broadband log-spiral antenna. For additional focusing ofthe incident radiation a silicon hyperhemispherical lens was used. For the 0.1–30 THz receivingsystem, the sensitive element was patterned as parallel strips(2μm wide each) filling an area of 500×500μm2with a filling factor of 0.5. In the receivingsystem of this type we used direct coupling of the incident radiation to the sensitive element. Inthe 25–70 THz range (detector type 2/2a in Table 1) we used a square-shaped superconductingdetector with planar dimensions of 10×10μm2. Incident radiation was coupled to the detectorwith the use of a germanium hyperhemispherical lens.The response time of the above receiving systems is determined by the cooling rate of the hotelectrons in the film. That depends on the electron-phonon interaction time, which is less forultrathin NbN than in MoRe.
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Treuttel, J., Thomas, B., Maestrini, A., Wang, H., Alderman, B., Siles, J. V., et al. (2009). A 380 GHz sub-harmonic mixer using MMIC foundry based Schottky diodes transferred onto quartz substrate. In Proc. 20th Int. Symp. Space Terahertz Technol.. Charlottesville, Virginia, USA.
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Meledin, D., Pavolotsky, A., Desmaris, V., Lapkin, I., Risacher, C., Perez, V., et al. (2009). A 1.3-THz balanced waveguide HEB mixer for the APEX telescope. IEEE Trans. Microw. Theory Techn., 57(1), 89–98.
Abstract: In this paper, we report about the development, fabrication, and characterization of a balanced waveguide hot electron bolometer (HEB) receiver for the Atacama Pathfinder EXperiment telescope covering the frequency band of 1.25–1.39 THz. The receiver uses a quadrature balanced scheme and two HEB mixers, fabricated from 4- to 5-nm-thick NbN film deposited on crystalline quartz substrate with an MgO buffer layer in between. We employed a novel micromachining method to produce all-metal waveguide parts at submicrometer accuracy (the main-mode waveguide dimensions are 90×180 μm). We present details on the mixer design and measurement results, including receiver noise performance, stability and “first-light†at the telescope site. The receiver yields a double-sideband noise temperature averaged over the RF band below 1200 K, and outstanding stability with a spectroscopic Allan time more than 200 s.
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