New designs of survey telescopes

Terebizh, V. Yu.

doi:10.1002/asna.201111576

Cited by 23 publications

(27 citation statements)

References 77 publications

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“…G max ≃ 31.25 ε 2 (D/|R 0 |) 3 , µm/mm (Terebizh 2011). For mirrors, it is simpler to use the equivalent formula:…”

Section: Discussionmentioning

confidence: 99%

Space Telescope Designed for Accurate Measurements

Terebizh¹

2017

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A modified version of the folded aplanatic Gregory telescope equipped with a spherical two-lens corrector is proposed for observations requiring a high signal-to-noise ratio. The basic telescope model has an aperture of 400 mm (f/3.0), its field of view is 3. • 0, the linear obscuration is 0.12, the distortion is less than 0.5%. The focal surface has a spherical shape; the achieving of a plane field requires an increase in the number of lenses in the corrector. The images of stars in the integrated wavelength range 0.35 -1.0 µm are close to the diffractionlimited ones (D 80 = 5.9 -8.2 µm = 1. ′′ 0 -1. ′′ 4). The system is free from direct background illumination; both the lens corrector and the light detector are protected from cosmic particles. *

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“…G max ≃ 31.25 ε 2 (D/|R 0 |) 3 , µm/mm (Terebizh 2011). For mirrors, it is simpler to use the equivalent formula:…”

Section: Discussionmentioning

confidence: 99%

Space Telescope Designed for Accurate Measurements

Terebizh¹

2017

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“…As a wide angle telescope for the EKOZONT sys tem we propose to use the analog of the VT 77h system proposed by V. Terebizh [14]. Considered as a mirror lens system with a full aperture input corrector, it is a modified version of the Richter-Slevogt scheme.…”

Section: The System Compositionmentioning

confidence: 99%

On the concept of a low-cost space system for detecting hazardous celestial bodies

et al. 2015

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“…2 gives an idea of the telescope aperture D and the angular field of view diameter 2w for systems listed in Table 1. As in the much more extensive set of existing telescopes discussed by Terebizh (2011), the field of view size is, to a first approximation, inversely proportional to the aperture diameter: 2w…”

Section: Optical Layouts 21 Flat Focal Surfacementioning

confidence: 99%

“…An adequate measure of survey efficiency, the sky survey rate Γ, was proposed by V.V. Biryukov and the author (Terebizh 2011). In the case when the dead time is much less than the exposure time, the sky survey rate is proportional to the ratio of the observed sky area πw 2 to the exposure time, needed to achieve the required S/N value.…”

Section: Sky Survey Ratementioning

confidence: 99%

On the Capabilities of Survey Telescopes of Moderate Size

Terebizh

2016

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To explore capabilities of moderate-size optical telescopes in surveys, the set of 9 new wide-field designs having apertures up to 1 m is considered. All but one systems have angular field of view in a range 3.5 • −10 • and flat focal surface; the field of the last system is 45 • in diameter at the 0.5 m aperture and spherical focal surface. The complete description of the optical layouts is given in the Appendix. Relations between the expected limiting magnitude, survey speed and exposure time allow to choose the system that is most suitable for a particular task of observations. In principle, a single wide-field telescope with the aperture of approximately 1 m can detect objects brighter than 22.5 m over the entire hemisphere within one night, however, the reliability of acquired data can be significantly increased by using a hierarchic observational network comprised of telescopes with optimized parameters.

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New designs of survey telescopes

Cited by 23 publications

References 77 publications

Space Telescope Designed for Accurate Measurements

Space Telescope Designed for Accurate Measurements

On the concept of a low-cost space system for detecting hazardous celestial bodies

On the Capabilities of Survey Telescopes of Moderate Size

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