The 10 references with contexts in paper D. Kozhevnikov A., R. Fiodоrtsev V., A. Silie r, Д. Кожевников А., Р. Фёдорцев В., А. Силие Р. (2018) “Орбитальный телескоп с синтезированной апертурой для аппаратуры дистанционного зондирования Земли // Synthetic Aperture Orbital Telescope for Earth Remote Sensing Equipment” / spz:neicon:pimi:y:2018:i:4:p:280-287

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Sharing Earth Observation Resources. eoPortal Directory. Satellite Missions. European Space Agency. ESA 2000-2018. Available at: https://earth.esa.int/web/ eoportal/satellite-missions
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    of the optical-electronic systems of a spacecraft is determined by the atmospheric transparency windows in the visible (380–720 nm) and near infrared (720–1300 nm) spectral regions. Some sensors of some satellites (for example, IRS-P6 or SPOT 5) use the middle infrared range (up to 1.75 μm) or the far infrared range 10.4– 12.5 μm (Landsat 7 ETM +) (Table 1)
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    . The spatial resolution determines the smallest size of objects that can be distinguished in the image and can be carried out both in panchromatic mode (more accurate) and in multispectral mode.

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QuickBird Imagery Products. Product Guide. DigitalGlobe, Inc. Revision 4.7.1. Release Date: 1 May 2006, 78 p.
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    of the optical-electronic systems of a spacecraft is determined by the atmospheric transparency windows in the visible (380–720 nm) and near infrared (720–1300 nm) spectral regions. Some sensors of some satellites (for example, IRS-P6 or SPOT 5) use the middle infrared range (up to 1.75 μm) or the far infrared range 10.4– 12.5 μm (Landsat 7 ETM +) (Table 1)
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    . The spatial resolution determines the smallest size of objects that can be distinguished in the image and can be carried out both in panchromatic mode (more accurate) and in multispectral mode.

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Kobernichenko V.G., Trenikhin V.A. [Methods of image synthesis based on remote sensing data of the earth of various resolutions]. Successes of modern radio electronics, 2007, no. 4, pp. 22–31 (in Russian).
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    The spatial resolution determines the smallest size of objects that can be distinguished in the image and can be carried out both in panchromatic mode (more accurate) and in multispectral mode. Today, ultra-high-resolution images include images in which objects of 0.3–0.9 m in size are visible
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    . The actual task remains to increase the temporal resolution, which determines the frequency of obtaining images of a specific area on the earth's surface. For existing space remote sensing satellites, the best spatial resolution is 1–3 days.

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Malinnikov V.A., Stetsenko A.F., Altynov A.E., Popov S.M. Monitoring prirodnoy sredi aerokosmicheskimi sredstwami [Monitoring the natural environment by aerospace tools], Moscow, MIIGAiK Publ., 2008, 173 p. (in Russian).
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    For existing space remote sensing satellites, the best spatial resolution is 1–3 days. In this case, the duration of observation for one surface area is limited to a time interval of not more than 1 min
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    . However, there are a number of areas that require almost continuous surveys for a sufficiently long period of time (for example, meteorology – during the development of cyclones and hurricanes, agriculture – monitoring of areas covered by forest fires, as well as the military area and antiterrorist operations for tracking facilities that pose a pot

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Demin A.V. Mathematical model of the process of adjustment of composite mirrors // News of universities. Instrument making. – 2015. – Vol. 58, no. 11, pp. 901–907 (in Russian). DOI: 10.17586/0021-3454-2015-58-11-901-907
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    In addition, technological costs associated with the formation of a high-quality reflective surface increase. Creating systems with a large aperture was made possible by splitting the main mirror into segments
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    . According to the theory, in a synthesized aperture telescope, the final image is formed from separate fragments of several mirror modules and is equivalent in quality to a telescope with a solid mirror surface, provided that the images are geographically acceptable and phase synchronized.

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Curtis Baffes, Terry Mast, Jerry Nelson, Eric Ponslet, Vince Stephens, Larry Stepp, Eric C. Williams. Primary Mirror Segmentation Studies for the Thirty Meter Telescope. SPIE 7018-29, TMT.OPT.JOU.08.003. REL01, JPL CL#08-1541. – 15 p.
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    In addition, technological costs associated with the formation of a high-quality reflective surface increase. Creating systems with a large aperture was made possible by splitting the main mirror into segments
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    . According to the theory, in a synthesized aperture telescope, the final image is formed from separate fragments of several mirror modules and is equivalent in quality to a telescope with a solid mirror surface, provided that the images are geographically acceptable and phase synchronized.

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Sabelhaus P.A., Decker J.E. An overview of the James Webb Space Telescope (JWST) project. Proceeding of SPIE, 2004, vol. 5487, 14 p. DOI: 10.1117/12.549895
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    been successfully solved only for ground-based observatories: the Very Large Telescope of the South European Observatory (VLT ESO); Hopkins multi-mirror telescope (MZT) and mainly for radar systems (Murchison Radio Astronomy Observatory, ASKAP). Orbital telescopes with segmented elements of the main mirror are implemented only in James Webb Space Telescope (JWST)
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    . Design options for orbital telescopes with synthetic aperture are currently lacking. The purpose of the research was to develop a concept and determine possible options for building a high-resolution orbital telescope with a synthesized aperture of the main mirror for a remote sensing satellite located in a geostationary orbit.

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Demin A.V., Kovalev I.A. The Mathematical model and the simulation modelling algorithm of the multitiered mechanical system. ABC Journal of Advanced Research, 2013, мol. 2(1), is. 3, pp. 44–48. DOI: 10.18034/abcjar.v2il.427
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    In addition, the tilt of the image causes a phase shift of the light oscillations, which leads to disruption of the phase conjugation of the folding wavefronts. The formation of a synthesized aperture by combining individual power modules provides a relatively low image quality (at m0 = 1 m, and W = 1'', W00ji = 10 μm)
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    . The main advantage of afocal systems is to maintain the parallelism of the beams after passing through the modules – there is no image tilt. In this regard, to project an image onto a photodetector, a collector telescopic system is needed, to which high demands are made.

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Gardner J.P., Mather J.C., Clampin M., Doyon R., Greenhouse M.A., Hammel H.B., Wright G.S. The James Webb space telescope. Space Science Reviews, 2006, vol. 123(4), pp. 485-606. DOI: https://doi.org/10.1007/ s11214-006-8315-7
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    and adjustment Precise mirror curvature setting automatically High complexity of the adjustment of individual modules and their system relative to the receiver, requiring special equipment The adjustment difficulty is high, but fewer parameters are being monitored than in the system with power modules Cost coefficient1**0.76**0.84* Weightm = 300–800 kgm/γ***m/0.8γ*** * JWST compliant
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    ** according to the source [10] *** γ – the ratio of the diameter of the equivalent aperture to the diameter of the module 285 circle with a diameter of Deq = 3500 mm. The diameter of the main mirror of the module is set to Dmod = 800 mm, taking into account the need to observe intermodular gaps ∆N1.

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Ermolaeva E.V., Zverev V.A., Filatov A.A. Adaptivnaya optika [Adaptive optics]. – SPb: NRU ITMO, 2012. – 297 p. (in Russian). 287
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    curvature setting automatically High complexity of the adjustment of individual modules and their system relative to the receiver, requiring special equipment The adjustment difficulty is high, but fewer parameters are being monitored than in the system with power modules Cost coefficient1**0.76**0.84* Weightm = 300–800 kgm/γ***m/0.8γ*** * JWST compliant [9] ** according to the source
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    *** γ – the ratio of the diameter of the equivalent aperture to the diameter of the module 285 circle with a diameter of Deq = 3500 mm. The diameter of the main mirror of the module is set to Dmod = 800 mm, taking into account the need to observe intermodular gaps ∆N1.