Shape accuracy requirements on starshades for large and small apertures

Shaklan, Stuart; Marchen, Luis; Cady, Eric

doi:10.1117/12.2273436

Cited by 6 publications

(8 citation statements)

References 2 publications

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“…The starshade design considered here has ∼100% optical throughput at the IWA. 24 Although it is, in principle, possible to observe targets at angles below the IWA, the throughput is reduced and the PSF is distorted. For practical purposes, we assume exoplanets are only observable at angles above the IWA.…”

Section: Starshadementioning

confidence: 99%

Starshade rendezvous: exoplanet sensitivity and observing strategy

Romero-Wolf

Bryden

Seager

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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Section: Starshadementioning

confidence: 99%

Starshade rendezvous: exoplanet sensitivity and observing strategy

Romero-Wolf

Bryden

Seager

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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“…The topic is complicated by geometry descriptions, statistical correlations, and averaging due to spinning. 16 Numerical study of this is beyond the scope of this initial work. Yet, recall that once an areal quadrature exists for the desired shape Ω, the proposed method is very simple.…”

Section: Application To Non-ideal (Perturbed) Starshadesmentioning

confidence: 97%

“…In Fig. 5, we compare the wave amplitudes along a radial slice computed by three methods for two designs of starshade: "NI2" (a small occulter with rippled profile optimized for a bluegreen λ range 16 ) and "HG" (a large occulter with analytic "offset hyper-Gaussian" profile 14 ). We choose λ within their designed wavelength windows.…”

Section: Accuracy Validationmentioning

confidence: 99%

“…One motivation is starshade design. 10,[13][14][15][16][17] Given a space telescope, the goal is that a distant binary occulter blocks the direct light from a star, allowing for much dimmer exoplanets separated from it by only tens of milli-arcseconds to be imaged. The occulter shape and distance are thus optimized to give a deep shadow region, with a relative intensity on the order of 10 −10 across the telescope pupil, throughout a given wavelength range, while minimizing the occulter's physical size (for practical reasons) and the angular size at the telescope.…”

Section: Introductionmentioning

confidence: 99%

“…Numerical modeling is challenging, demanding at least 6-digit accuracy in amplitude to validate the shadow and many runs with different wavelengths and shapes to assess mechanical and thermal stability. 16 Fixing a wavelength λ and propagation distance z, a point in the aperture (or occulter) plane is ðx; y; 0Þ and a target point in the detector (or pupil) plane is ðξ; η; zÞ (see Fig. 1).…”

Section: Introductionmentioning

confidence: 99%

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Efficient high-order accurate Fresnel diffraction via areal quadrature and the nonuniform fast Fourier transform

Barnett

2021

J. Astron. Telesc. Instrum. Syst.

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We present a fast algorithm for computing the diffracted field from arbitrary binary (sharp-edged) planar apertures and occulters in the scalar Fresnel approximation for up to moderately high Fresnel numbers (≲10 3). It uses a high-order areal quadrature over the aperture and then exploits a single 2D nonuniform fast Fourier transform to evaluate rapidly at target points (on the order of 10 7 such points per second, independent of aperture complexity). It thus combines the high accuracy of edge integral methods with the high speed of Fourier methods. Its cost is Oðn 2 log nÞ, where n is the linear resolution required in the source and target planes, to be compared with Oðn 3 Þ for edge integral methods. In tests with several aperture shapes, this translates to between two and five orders of magnitude acceleration. In starshade modeling for exoplanet astronomy, we find that it is roughly 10 4 × faster than the state-of-the art in accurately computing the set of telescope pupil wavefronts. We provide a documented, tested MATLAB/ Octave implementation. An appendix shows the mathematical equivalence of the boundary diffraction wave, angular integration, and line integral formulas and then the analysis of a new nonsingular reformulation that eliminates their common difficulties near the geometric shadow edge. This supplies a robust edge integral reference against which to validate the main proposal. © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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Special Section on Starshades: Overview and a Dialogue

Arenberg

Harness

Jensen-Clem

2021

J. Astron. Telesc. Instrum. Syst.

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This special section is dedicated to starshades: science, engineering, technology, and programmatics. Our reasons for organizing this special section are several fold. First as a new technology and with research accomplished in many institutions, recent results are widely scattered in the literature. As such, we see great value in colocating many of the most recent results. This guest editorial summarizes the 19 contributed papers as the result of a special call for papers. Since this is a rapidly maturing technology, we wanted to colocate a primer with the most current work in the field. It is hoped that this primer will provide a tutorial to the starshade concept and pathway to the literature not in this section. In doing so, we hope to widen the starshade community in terms of engineering and scientific engagements. This tutorial takes the form of a dialogue, where frequently asked questions are answered.

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Shape accuracy requirements on starshades for large and small apertures

Cited by 6 publications

References 2 publications

Starshade rendezvous: exoplanet sensitivity and observing strategy

Starshade rendezvous: exoplanet sensitivity and observing strategy

Efficient high-order accurate Fresnel diffraction via areal quadrature and the nonuniform fast Fourier transform

Special Section on Starshades: Overview and a Dialogue

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