Spectral Response of Arrays of Half-wave and Electrically Small Antennas with SINIS Bolometers
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Spectral Response of Arrays of Half-wave and Electrically Small Antennas with SINIS Bolometers A. A. Gunbinaa, b, *, M. A. Tarasovc, S. A. Lemzyakovd, e, A. M. Chekushkinc, R. A. Yusupovc, D. V. Nagirnayac, M. A. Mansfel’da, b, V. F. Vdovina, b, D. Winkler f, A. S. Kalaboukhov f, S. Mahashabde f, and V. S. Edel’mand a Institute
of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russia b Alekseev State Technical University, Nizhny Novgorod, Russia c Kotelnikov Institute of Radio Engineering and Electronics, Russian Academy of Sciences, Moscow, Russia d Kapitza Institute for Physical Problems, Russian Academy of Sciences, Moscow, Russia e Moscow Institute of Physics and Technology, Dolgoprudny, Moscow oblast, Russia f Chalmers University of Technology, Göteborg, Sweden *e-mail: [email protected] Received March 26, 2020; revised March 26, 2020; accepted April 2, 2020
Abstract—Two types arrays of annular half-wave and electrically small antennas with typical sizes of the elements corresponding to 1/10 of the wavelength at SubTHz band with integrated superconductor–insulator– normal metal–insulator–superconductor (SINIS) bolometers have been developed, fabricated and experimentally studied. We performed numerical modeling of the full structure and use additional reference channels in experimental studies to enhance the accuracy of the spectral response estimations of receiving arrays. In experiments three reference channels were used for normalization of the spectral response: a pyroelectric detector outside the cryostat, and two cold channels—a RuO2 bolometer and on-chip thermometer comprising series array of NIS-junctions. Keywords: SINIS-bolometers, arrays of planar antennas, terahertz radiation DOI: 10.1134/S1063783420090097
1. INTRODUCTION Astronomic observations in the millimeter and submillimeter bands [1] become topical over recent years, there have appeared a demand in high sensitive receiving systems based on cooled bolometers. Such systems have contradictory requirements: the noise equivalent power (NEP) should be at least 10‒16 W/Hz1/2 for ground-based and by three orders of magnitude better for space observatories with a wide dynamic range for operation under conditions of a relatively high background power (tens of pW for groundbased observatories). At present time the most advanced and widely used types are transition edge sensors (TES) [2, 3] and kinetic inductance detectors (KID) [4, 5]. TES have high sensitivity, but their dynamic range is narrow, rate is low, and operation requires high stability of the bath temperature. The main advantage of KIDs is a low level of intrinsic noise due to the absence of the Nyquist noise, but the absolute value of the kinetic inductance response is low. In the superconductor–insulator–normal metal–insulator–superconductor (SINIS) [6, 7] bolometers presented in this study these disadvantages were over-
come. A single SINIS bolometer is saturated at a power level about 1 pW. Therefore, such bolometers are connected into arrays so a
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