Pair-wise, deformable mirror, image plane-based diversity electric field estimation for high contrast coronagraphy

Give’on, Amir; Kern, Brian; Shaklan, Stuart

doi:10.1117/12.895117

Cited by 66 publications

(77 citation statements)

References 7 publications

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“…The exact number has some chromatic dependence, and decorrelates from the coherent signal entirely. (This behavior was also noted in [1]. )…”

Section: Discussionsupporting

confidence: 57%

“…These settings are selected in accordance with the procedure suggested in [1], using two positive and negative versions of two independent probe settings and a fifth unprobed image. The appendix to this paper also describes the methodology, though it does not delve into the motivation as [1] does.…”

Section: Filtering/post-processingmentioning

confidence: 99%

“…At the High Contrast Imaging Testbed (HCIT) at NASA/JPL, we use primarily a pairwise-estimation scheme which modulates the electric field by applying known offsets to the deformable mirror settings. A comprehensive description is given in [1]. (Subsequent correction is an orthogonal problem; the HCIT control software uses electric field conjugation [2], but other methods, such as speckle nulling [3], could used without requiring any changes.…”

Section: Introductionmentioning

confidence: 99%

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Measurements of incoherent light and background structure at exo-Earth detection levels in the High Contrast Imaging Testbed

Cady

Shaklan

2014

SPIE Proceedings

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A major component of the estimation and correction of starlight at very high contrasts is the creation of a dark hole: a region in the vicinity of the core of the stellar point spread function (PSF) where speckles in the PSF wings have been greatly attenuated, up to a factor of 10 10 for the imaging of terrestrial exoplanets. At these very high contrasts, removing these speckles requires distinguishing between light from the stellar PSF scattered by instrument imperfections, which may be partially corrected across a broad band using deformable mirrors in the system, from light from other sources which generally may not. These other sources may be external or internal to the instrument (e.g. planets, exozodiacal light), but in either case, their distinguishing characteristic is their inability to interfere coherently with the PSF. In the following we discuss the estimation, structure, and expected origin of this "incoherent" signal, primarily in the context of a series of experiments made with a linear band-limited mask in Jan-Mar 2013. We find that the "incoherent" signal at moderate contrasts is largely estimation error of the coherent signal, while at very high contrasts it represents a true floor which is stable over week-timescales.

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“…The exact number has some chromatic dependence, and decorrelates from the coherent signal entirely. (This behavior was also noted in [1]. )…”

Section: Discussionsupporting

confidence: 57%

Section: Filtering/post-processingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Measurements of incoherent light and background structure at exo-Earth detection levels in the High Contrast Imaging Testbed

Cady

Shaklan

2014

SPIE Proceedings

Self Cite

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“…The effect of probe uncertainty is minimized by measuring the probe amplitude directly as explained in Ref. 29, but its phase must still be obtained from the model. One can always use Eq.…”

Section: Maximum Allowable Probe Brightnessmentioning

confidence: 99%

Methods and limitations of focal plane sensing, estimation, and control in high-contrast imaging

Groff

Riggs

Kern

et al. 2015

J. Astron. Telesc. Instrum. Syst

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Abstract. Coronagraphy is a very promising method for directly imaging exoplanets, but the performance of a coronagraph is highly sensitive to quasi-static aberrations within the telescope. The resultant speckles are suppressed in the final focal plane using a wavefront control system that estimates the field at the final focal plane to avoid any noncommon path error. This requires a set of probe images that modulate the field so that it may be estimated. With an estimate of the focal plane electric field, a control law is defined to suppress the speckle field so that the planet can be imaged. Characterizing the planet requires that the speckle field be suppressed simultaneously over the bandpass of interest. The choice of control law, bandpass, estimator, and probing methodology has implications in the control solutions and contrast performance. Here, we compare wavefront probing, estimation, and control algorithms, and describe their practical implementation. © 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)

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“…The Electric Field Conjugation algorithm (EFC) is well described in [26,27]. This algorithm needs an estimation of the amplitude of the electric field in the focal plane.…”

Section: Electric Field Conjugationmentioning

confidence: 99%

Comparison of wavefront control algorithms and first results on the high-contrast imager for complex aperture telescopes (hicat) testbed

Leboulleux

N’Diaye

Mazoyer

et al. 2017

International Conference on Space Optics — ICSO 2016

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Pair-wise, deformable mirror, image plane-based diversity electric field estimation for high contrast coronagraphy

Cited by 66 publications

References 7 publications

Measurements of incoherent light and background structure at exo-Earth detection levels in the High Contrast Imaging Testbed

Measurements of incoherent light and background structure at exo-Earth detection levels in the High Contrast Imaging Testbed

Methods and limitations of focal plane sensing, estimation, and control in high-contrast imaging

Comparison of wavefront control algorithms and first results on the high-contrast imager for complex aperture telescopes (hicat) testbed

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