On the Capabilities of Survey Telescopes of Moderate Size

Terebizh, V. Yu.

doi:10.3847/0004-6256/152/5/121

Cited by 9 publications

(3 citation statements)

References 25 publications

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“…A number of papers have been written about sky survey design and optimization including Tonry (2011), Terebizh (2011Terebizh ( , 2016, and Bellm (2016). Tonry (2011) summarized survey performance in terms of a "survey speed" that expresses the rate at which objects can be observed to a limiting magnitude m with signal to noise ratio SNR.…”

Section: Introductionmentioning

confidence: 99%

ATLAS: A High-cadence All-sky Survey System

Tonry¹,

Denneau²,

Heinze³

et al. 2018

PASP

831

609

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Technology has advanced to the point that it is possible to image the entire sky every night and process the data in real time. The sky is hardly static: many interesting phenomena occur, including variable stationary objects such as stars or QSOs, transient stationary objects such as supernovae or M dwarf flares, and moving objects such as asteroids and the stars themselves. Funded by NASA, we have designed and built a sky survey system for the purpose of finding dangerous near-Earth asteroids (NEAs). This system, the "Asteroid Terrestrial-impact Last Alert System" (ATLAS), has been optimized to produce the best survey capability per unit cost, and therefore is an efficient and competitive system for finding potentially hazardous asteroids (PHAs) but also for tracking variables and finding transients. While carrying out its NASA mission, ATLAS now discovers more bright (m < 19) supernovae candidates than any ground based survey, frequently detecting very young explosions due to its 2 day cadence. ATLAS discovered the afterglow of a gamma-ray burst independent of the high energy trigger and has released a variable star catalogue of 5×10 6 sources. This is the first of a series of articles describing ATLAS, devoted to the design and performance of the ATLAS system. Subsequent articles will describe in more detail the software, the survey strategy, ATLAS-derived NEA population statistics, transient detections, and the first data release of variable stars and transient lightcurves.

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Section: Introductionmentioning

confidence: 99%

ATLAS: A High-cadence All-sky Survey System

Tonry¹,

Denneau²,

Heinze³

et al. 2018

PASP

831

609

View full text Add to dashboard Cite

show abstract

“…Wide-field corrector is added to the prime-focus optical system to further correct aberrations and expand the FOV. The optical design result is Terebizh-style [29] with five spherical lenses, as shown in Figure 8 and Table 5.…”

Section: Optical System Design Resultsmentioning

confidence: 99%

Optical system design method of the all-day starlight refraction navigation system

Wu,

Wang,

Yan

2023

J. Eur. Opt. Society-Rapid Publ.

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The application of starlight refraction navigation to spacecraft and space weapons is a significant development direction. Observing enough refracted stars for the star sensor in a strong limb background is an urgent problem. The all-day optical system parameters are analyzed based on the star detection requirement and navigation accuracy. Combined with primary aberration theory, the prime-focus catadioptric optical system is selected to meet the design requirements of a wide field of view (FOV) and tight structure. An H-band (1.52um-1.78um) star sensor is designed with a FOV of 6°, a focal length of 831mm, an effective aperture of 253mm, and a relative distortion of 0.03%. The energy concentration of the star point is 85% within 30um, and the maximum lateral chromatic aberration is 2.9um, which meets the imaging requirements. Furthermore, a baffle is designed to avoid the influence of direct sunlight on stellar imaging. The proposed method can provide a theoretical foundation and technical support for the optical design of the refraction star navigation.

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“…Obviously, in these conditions it is not easy to find a suitable solution both in the class of axisymmetrical wide-field systems (Terebizh 2011(Terebizh , 2016) and among off-axial systems with aspheric and freeform optical surfaces (Hugot et al 2014;Buffington 1998;Singaravelu and Cabanac 2014;Challita et al 2014). In this note, we consider a 400-mm model, which is a modified version of the folded aplanatic Gregory telescope 1 provided by a two-lens corrector protected from cosmic particles.…”

Section: Introductionmentioning

confidence: 99%

Space Telescope Designed for Accurate Measurements

Terebizh¹

2017

Self Cite

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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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On the Capabilities of Survey Telescopes of Moderate Size

Cited by 9 publications

References 25 publications

ATLAS: A High-cadence All-sky Survey System

ATLAS: A High-cadence All-sky Survey System

Optical system design method of the all-day starlight refraction navigation system

Space Telescope Designed for Accurate Measurements

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