Probability of getting a lucky short-exposure image through turbulence*

Fried, David L.

doi:10.1364/josa.68.001651

Cited by 305 publications

(170 citation statements)

References 3 publications

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“…Occasionally the combined phase variations across the telescope aperture, δ, due to the atmosphere and mirror, will be small (<∼ 1 radian). The corresponding image of a star will have a core which is diffraction-limited with a Strehl ratio of exp (−δ 2 ) and angular resolution 1.22λ/D determined by the aperture diameter D. Fried (1978) calculated the probability, P , of "lucky exposures" having phase variations less than 1 radian across an aperture diameter D for seeing defined by r 0 :…”

Section: Introductionmentioning

confidence: 99%

Diffraction-limited 800 nm imaging with the 2.56 m Nordic Optical Telescope

Baldwin¹,

Tubbs²,

Cox³

et al. 2001

A&A

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Section: Introductionmentioning

confidence: 99%

Diffraction-limited 800 nm imaging with the 2.56 m Nordic Optical Telescope

Baldwin¹,

Tubbs²,

Cox³

et al. 2001

A&A

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“…A selection of high-quality frames should also be performed among the whole data set to improve the signal-to-noise ratio by using, for instance, merit functions (Patru et al 2017). A drastic selectionin a lucky imaging mode (Fried 1978) -would allow us to directly detect a compagnon located in a high-gain zone. In particular, we would recommend to adapt an ADI-like technique for searching extrasolar planets, taking advantage of the numerous high-contrast gain zones.…”

Section: O N C L U S I O Nmentioning

confidence: 99%

The LBTI Fizeau imager – I. Fundamental gain in high-contrast imaging

Patru

Esposito

Puglisi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We show by numerical simulations a fundamental gain in contrast when combining coherently monochromatic light from two adaptive optics (AO) telescopes instead of using a single stand-alone AO telescope, assuming efficient control and acquisition systems at high speed. A contrast gain map is defined as the normalized point spread functions (PSFs) ratio of a single Large Binocular Telescope (LBT) aperture over the dual Large Binocular Telescope Interferometer (LBTI) aperture in Fizeau mode. The global gain averaged across the AO-corrected field of view is improved by a factor of 2 in contrast in long exposures and by a factor of 10 in contrast in short exposures (i.e. in exposures, respectively, longer or shorter than the coherence time). The fringed speckle halo in short exposures contains not only highangular resolution information, as stated by speckle imaging and speckle interferometry, but also high-contrast imaging information. A high-gain zone is further produced in the valleys of the PSF formed by the dark Airy rings and/or the dark fringes. Earth rotation allows us to exploit various areas in the contrast gain map. A huge-contrast gain in narrow zones can be achieved when both a dark fringe and a dark ring overlap on to an exoplanet. Compared to a single 8-m LBT aperture, the 23-m LBTI Fizeau imager can provide a gain in sensitivity (by a factor of 4), a gain in angular resolution (by a factor of 3) and, as well, a gain in raw contrast (by a factor of 2-1000 varying over the AO-corrected field of view).Key words: instrumentation: adaptive optics -instrumentation: interferometers -methods: numerical -techniques: high angular resolution -techniques: interferometric. I N T RO D U C T I O NThe LBTI (Large Binocular Telescope Interferometer; Angel & Woolf 1997;Angel et al. 1998;Herbst 2003;Hill et al. 2014;Hinz et al. 2014Hinz et al. , 2016 used in Fizeau mode can produce direct images by combining coherently the beams separated by a 14.4-m baseline from the two 8.4-m primary mirrors of the LBT (Large Binocular Telescope). Fizeau imaging can deliver the sensitivity of a 12-m telescope and the angular resolution of a 23-m telescope across the field of view provided by two adaptive optics (AO) systems. We show in this paper that, compared to a single stand-alone LBT aperture, the LBTI Fizeau imager can also significantly improve the raw contrast by means of two first light adaptive optics (FLAO)

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“…Lucky Imaging (Fried 1978) was performed in 2010 October and 2011 October using FastCam (Oscoz et al 2008) on the 1.5 m TCS telescope at Observatorio del Teide in Spain to search for companions at large separations from the primary star. Lucky Imaging consists of taking observations at very high cadence to achieve nearly diffraction-limited images from a subsample of the total.…”

Section: Imagingmentioning

confidence: 99%

Very Low Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Ii. A Short-Period Companion Orbiting an F Star With Evidence of a Stellar Tertiary and Significant Mutual Inclination

Fleming

Barnes

et al. 2012

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Probability of getting a lucky short-exposure image through turbulence*

Cited by 305 publications

References 3 publications

Diffraction-limited 800 nm imaging with the 2.56 m Nordic Optical Telescope

Diffraction-limited 800 nm imaging with the 2.56 m Nordic Optical Telescope

The LBTI Fizeau imager – I. Fundamental gain in high-contrast imaging

Very Low Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Ii. A Short-Period Companion Orbiting an F Star With Evidence of a Stellar Tertiary and Significant Mutual Inclination

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