V The Effects of Atmospheric Turbulence in Optical Astronomy

Roddier, F.

doi:10.1016/s0079-6638(08)70204-x

Cited by 743 publications

(595 citation statements)

References 182 publications

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“…It is experimentally proved by Nightingale & Buscher (1991) [8]. In case of atmospheric turbulence it is solar energy and wind shear which provides the initial energy on large scales and it is dissipated as heat by viscous friction of the air at the inner scale [9].…”

Section:   mentioning

confidence: 96%

A Study on atmospheric turbulence with Shearing Interferometer wavefront sensor

Ismail¹

2015

IJIRSET

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When a light beam propagates through the turbulent atmosphere, the wavefront of the beam is distorted, which affect the image quality of ground based telescopes. Adaptive optics is a means for real time compensation of the wavefront distortions. In an adaptive optics system, wavefront distortions are measured by a wavefront sensor, and then using an active optical element such as a deformable mirror the instantaneous wavefront distortions are corrected. In this paper, the physical background of imaging through turbulence, using Kolmogorov statistics, and the Polarization Shearing Interferometry techniques to sense and to correct the wavefront aberrations with adaptive optics have been discussed. Simulations of the interferometric records were carried out using Matlab for the study of aberrations in an optical system and the effect of the atmospheric turbulence in the interferograms. The data was reduced from the interferogram using Fourier Transform Technique and the wavefront was reconstructed from the wavefront slope data.

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Section:   mentioning

confidence: 96%

A Study on atmospheric turbulence with Shearing Interferometer wavefront sensor

Ismail¹

2015

IJIRSET

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“…To evaluate the level of performance of an AO system, the correlation time, also known as the Greenwood time delay is the most relevant parameter. It is defined as τ 0 = 0.314r 0 /v where v is the mean wind speed weighted by the turbulence profile along the line of sight [21]. This parameter sets the speed at which an AO system has to react to correct for the atmospheric turbulence.…”

Section: Characteristics Of Images Distorted By the Atmospheric Turbumentioning

confidence: 99%

Adaptive Optics in High-Contrast Imaging

Milli¹,

Mawet²,

Mouillet³

et al. 2016

Astronomy at High Angular Resolution

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The development of adaptive optics (AO) played a major role in modern astronomy over the last three decades. By compensating for the atmospheric turbulence, these systems enable to reach the diffraction limit on large telescopes. In this review, we will focus on high contrast applications of adaptive optics, namely, imaging the close vicinity of bright stellar objects and revealing regions otherwise hidden within the turbulent halo of the atmosphere to look for objects with a contrast ratio lower than 10 −4 with respect to the central star. Such high-contrast AO-corrected observations have led to fundamental results in our current understanding of planetary formation and evolution as well as stellar evolution. AO systems equipped three generations of instruments, from the first pioneering experiments in the nineties, to the first wave of instruments on 8m-class telescopes in the years 2000, and finally to the extreme AO systems that have recently started operations. Along with highcontrast techniques, AO enables to reveal the circumstellar environment: massive protoplanetary disks featuring spiral arms, gaps or other asymetries hinting at ongoing planet formation, young giant planets shining in thermal emission, or tenuous debris disks and micron-sized dust leftover from collisions in massive asteroid-belt analogs. After introducing the science case and technical requirements, we will review the architecture of standard and extreme AO systems, before presenting a few selected science highlights obtained with recent AO instruments.

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“…We can derive the theoretical scintillation index as the integral of the scintillation power spectrum, W (f) (Roddier 1981),…”

Section: Scintillationmentioning

confidence: 99%

“…S(z, f) is the Fresnel filter function to account for the wavefront propagation and is given by sin 2 (πλzf 2 )/λ 2 (Roddier 1981), with λ being the wavelength of the light. It is this function that gives the intensity fluctuations an intrinsic spatial scale of r F = √ λz.…”

Section: Scintillationmentioning

confidence: 99%

Scintillation correction for astronomical photometry on large and extremely large telescopes with tomographic atmospheric reconstruction

Osborn

2014

Monthly Notices of the Royal Astronomical Society

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We describe a new concept to correct for scintillation noise on high-precision photometry in large and extremely large telescopes using telemetry data from adaptive optics (AO) systems. Most wide-field AO systems designed for the current era of very large telescopes and the next generation of extremely large telescopes require several guide stars to probe the turbulent atmosphere in the volume above the telescope. These data can be used to tomographically reconstruct the atmospheric turbulence profile and phase aberrations of the wavefront in order to assist wide-field AO correction. If the wavefront aberrations and altitude of the atmospheric turbulent layers are known from this tomographic model, then the effect of the scintillation can be calculated numerically and used to normalize the photometric light curve. We show through detailed Monte Carlo simulation that for an 8 m telescope with a 16 × 16 AO system we can reduce the scintillation noise by an order of magnitude.

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V The Effects of Atmospheric Turbulence in Optical Astronomy

Cited by 743 publications

References 182 publications

A Study on atmospheric turbulence with Shearing Interferometer wavefront sensor

A Study on atmospheric turbulence with Shearing Interferometer wavefront sensor

Adaptive Optics in High-Contrast Imaging

Scintillation correction for astronomical photometry on large and extremely large telescopes with tomographic atmospheric reconstruction

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