Abstract
The possibility of studying the radiation of discrete astronomical sources in the submilli-meter range of the spectrum using an on-board telescope is determined to a considerable extent by the threshold sensitivity of the instrument, which depends entirely on the size of the mirror and the threshold sensitivity of the radiation receiver. Estimates of the expected fluxes from sources [1] and of the efficiencies of telescope optical systems [2] show that with a mirror diameter of 1.5 m the radiation receiver must have a threshold sensitivity no worse than 10−11 W/Hz1/2 at a width of 1000 GHz for the region of sensitivity in order to reliably record the radiation of a number of interesting sources [1]. To cover the greatest possible part of the submillimeter range with one instrument it is desirable to use a wide-band receiver. The necessity of mounting the instrument on board a flying vehicle imposes a number of specific requirements: relatively small overall size, weight, and energy consumption and stability against vibrations and accelerations.
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Kobzev, A.A., Lapshin, V.I., Solomonov, S.V., Khaikin, A.S. (1976). A Two-Channel Cooled Receiver for On-Board Telescopes of the Submillimeter Range. In: Basov, N.G. (eds) Radio, Submillimeter, and X-Ray Telescopes. The Lebedev Physics Institute Series. Springer, Boston, MA. https://doi.org/10.1007/978-1-4899-2660-9_5
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DOI: https://doi.org/10.1007/978-1-4899-2660-9_5
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