Space optics: an introduction by the editors

Breckinridge, James B.; Wood, H. John

doi:10.1364/ao.32.001677

Cited by 5 publications

(2 citation statements)

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“…The early severe aberrations of HST's optical system were an important driver of phase-retrieval algorithms. Several efforts to characterise HST were published in an Applied Optics special issue (Breckinridge and Wood, 1993). Solving the phase-retrieval problem provides a reliable approach to characterise the optical system accurately.…”

Section: Parametric Psf Modelsmentioning

confidence: 99%

Point spread function modelling for astronomical telescopes: a review focused on weak gravitational lensing studies

Liaudat,

Starck,

Kilbinger

2023

Front. Astron. Space Sci.

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The accurate modelling of the point spread function (PSF) is of paramount importance in astronomical observations, as it allows for the correction of distortions and blurring caused by the telescope and atmosphere. PSF modelling is crucial for accurately measuring celestial objects’ properties. The last decades have brought us a steady increase in the power and complexity of astronomical telescopes and instruments. Upcoming galaxy surveys like Euclid and Legacy Survey of Space and Time (LSST) will observe an unprecedented amount and quality of data. Modelling the PSF for these new facilities and surveys requires novel modelling techniques that can cope with the ever-tightening error requirements. The purpose of this review is threefold. Firstly, we introduce the optical background required for a more physically motivated PSF modelling and propose an observational model that can be reused for future developments. Secondly, we provide an overview of the different physical contributors of the PSF, which includes the optic- and detector-level contributors and atmosphere. We expect that the overview will help better understand the modelled effects. Thirdly, we discuss the different methods for PSF modelling from the parametric and non-parametric families for ground- and space-based telescopes, with their advantages and limitations. Validation methods for PSF models are then addressed, with several metrics related to weak-lensing studies discussed in detail. Finally, we explore current challenges and future directions in PSF modelling for astronomical telescopes.

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Section: Parametric Psf Modelsmentioning

confidence: 99%

Point spread function modelling for astronomical telescopes: a review focused on weak gravitational lensing studies

Liaudat,

Starck,

Kilbinger

2023

Front. Astron. Space Sci.

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“…The Jet Propulsion Laboratory Wide-Field and Planetary Camera 2 (JPL WFIPC-2) has a pupil close to the 1-cm diameter secondary mirror where the correction for the HST primary mirror error was successfully placed. 3 Meinel and Meinel4 showed that the correction factor was related to the ratio of the primary mirror diameter to the exit pupil diameter. This means that the stable errors of an inflatable mirror can be corrected by a small element whose diameter is set by the required wavefront error (WFE) reduction factor.…”

Section: Upgrading To Visible Passband Requirementsmentioning

confidence: 99%

Inflation-deployed camera and hyper-thin mirrors

Breckinridge

Meinel

1998

Space Telescopes and Instruments V

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Inflatable optics have the potential for a large reduction in launch mass and volume, but they involve significant challenges to achieve the wavefront accuracy required for diffraction-limited operation in the visible and near JR. Current studies identify two major subsets of this topic: 1) inflation-deployed structures with a monolithic, but rolled, hyper-thin primary mirror and 2) an inflatable structure and inflatable membrane primary mirror. We address the current state of the art, the challenges involved, and a program development plan.

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Hubble Space Telescope Faint Object Camera calculated point-spread functions

Lyon¹,

Dorband²,

Hollis³

1997

Appl. Opt.

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A set of observed noisy Hubble Space Telescope Faint Object Camera point-spread functions is used to recover the combined Hubble and Faint Object Camera wave-front error. The low-spatial-frequency wave-front error is parameterized in terms of a set of 32 annular Zernike polynomials. The midlevel and higher spatial frequencies are parameterized in terms of set of 891 polar-Fourier polynomials. The parameterized wave-front error is used to generate accurate calculated point-spread functions, both pre- and post-COSTAR (corrective optics space telescope axial replacement), suitable for image restoration at arbitrary wavelengths. We describe the phase-retrieval-based recovery process and the phase parameterization. Resultant calculated precorrection and postcorrection point-spread functions are shown along with an estimate of both pre- and post-COSTAR spherical aberration.

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Space optics: an introduction by the editors

Cited by 5 publications

References 0 publications

Point spread function modelling for astronomical telescopes: a review focused on weak gravitational lensing studies

Point spread function modelling for astronomical telescopes: a review focused on weak gravitational lensing studies

Inflation-deployed camera and hyper-thin mirrors

Hubble Space Telescope Faint Object Camera calculated point-spread functions

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