The LUVOIR Extreme Coronagraph for Living Planetary Systems (ECLIPS) I: searching and characterizing exoplanetary gems

Pueyo, Laurent; Stark, Christopher C.; Juanola-Parramon, Roser; Zimmerman, Neil; Bolcar, Matthew R.; Roberge, Aki; Arney, Giada; Ruane, Garreth; Riggs, A. J. Eldorado; Belikov, Ruslan; Sirbu, Dan; Redding, Dave; Soummer, Rémi; Laginja, Iva; Will, Scott D.

doi:10.1117/12.2530722

Cited by 20 publications

(22 citation statements)

References 59 publications

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“…The analysis presented in this paper is statistical but static, i.e., without temporal evolution; the extension to dynamical drift rates depends on the observing scenario and wavefront control strategy, which will put the PASTIS propagation model on different time scales. 45,46 Future work will address such dynamic analysis methods for continuous WFS&C cases on ultra-stable telescopes.…”

Section: Discussionmentioning

confidence: 99%

“…In high-contrast coronagraphy, the best contrast is not typically obtained for the perfect aperture without any aberration, but more commonly in the presence of a wavefront control solution using deformable mirrors. 30,46 Therefore, we are studying the response of the coronagraphic system to a perturbation around that solution. Defining ϕ DH as the phase solution for best DH contrast and ϕ s as the segmented perturbation, the phase can be divided into E Q -T A R G E T ; t e m p : i n t r a l i n k -; e 0 0 2 ; 1 1 6 ; 1 3 1…”

Section: Matrix Formalism To Calculate the Average Dark Hole Contrastmentioning

confidence: 99%

“…[39][40][41] In particular, the direct effects of segmentation on the final coronagraphic contrast 42,43 are of interest in the context of high-contrast imaging, and there is an ongoing effort to characterize and quantify the requirements for such ultra-stable telescopes. [44][45][46][47] Studies performing Monte Carlo (MC) end-to-end (E2E) simulations 48,49 have confirmed the strict WFE requirements of a couple of tens of picometers over tens of minutes to enable the search for faint extra-solar planets, and analytical methods for the derivation of coronagraphic performance specifications have been proposed. 50,51 One thing that all of these studies have in common is that they define global WFE tolerances over the entire telescope pupil, where the segments have a random contribution to the overall aberrations.…”

Section: Introductionmentioning

confidence: 99%

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Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

Laginja

Soummer

Mugnier

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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This paper introduces an analytical method to calculate segment-level wavefront error (WFE) tolerances to enable the detection of faint extra-solar planets using segmentedaperture telescopes in space. This study provides a full treatment of the case of spatially uncorrelated segment phasing errors for segmented telescope coronagraphy, which has so far only been approached using ad-hoc Monte Carlo (MC) simulations. Instead of describing the wavefront tolerance globally for all segments, our method produces spatially dependent requirement maps. We relate the statistical mean contrast in the coronagraph dark hole to the standard deviation of the WFE of each individual segment on the primary mirror. This statistical framework for segment-level tolerancing extends the Pair-based Analytical model for Segmented Telescope Imaging from Space (PASTIS), which is based uniquely on a matrix multiplication for the optical propagation. We confirm our analytical results with MC simulations of end-to-end optical propagations through a coronagraph. Comparing our results for the Apodized Pupil Lyot Coronagraph designs for the Large Ultraviolet Optical Infrared telescope to previous studies, we show general agreement but we provide a relaxation of the requirements for a significant subset of segments in the pupil. These requirement maps are unique to any given telescope geometry and coronagraph design. The spatially uncorrelated segment tolerances we calculate are a key element of a complete error budget that will also need to include allocations for correlated segment contributions. We discuss how the PASTIS formalism can be extended to the spatially correlated case by deriving the statistical mean contrast and its variance for a nondiagonal aberration covariance matrix. The PASTIS tolerancing framework therefore brings a new capability that is necessary for the global tolerancing of future segmented space observatories.

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Section: Discussionmentioning

confidence: 99%

Section: Matrix Formalism To Calculate the Average Dark Hole Contrastmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

Laginja

Soummer

Mugnier

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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“…The numerical simulation generates images for each of the 8000 OPD time steps with PROPER 12 in a 20% bandwidth around 550nm and using the optimized Apodized Pupil Lyot Coronagraph (APLC). 3,13 For time series B, we find a mean intensity in the dark hole (DH) region, normalized by the maximum of the unocculted PSF, of 9.45 × 10 −11 . Comparing this result with the normalized intensity induced by sample B that is reduced to its first 10 principal components, the mean difference between the normalized intensity at each time steps is 4.2 × 10 −13 and standard deviation of the differences is 8.8 × 10 −13 .…”

Section: Contrast Calculation Using Principle Components Statisticsmentioning

confidence: 99%

LUVOIR-ECLIPS closed-loop adaptive optics performance and contrast predictions

Potier

Ruane

Chen

et al. 2021

Preprint

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One of the primary science goals of the Large UV/Optical/Infrared Surveyor (LUVOIR) mission concept is to detect and characterize Earth-like exoplanets orbiting nearby stars with direct imaging. The success of its coronagraph instrument ECLIPS (Extreme Coronagraph for Living Planetary Systems) depends on the ability to stabilize the wavefront from a large segmented mirror such that optical path differences are limited to tens of picometers RMS during an exposure time of a few hours. In order to relax the constraints on the mechanical stability, ECLIPS will be equipped with a wavefront sensing and control (WS&C) architecture to correct wavefront errors up to temporal frequencies 1 Hz. These errors may be dominated by spacecraft structural dynamics exciting vibrations at the segmented primary mirror. In this work, we present detailed simulations of the WS&C system within the ECLIPS instrument and the resulting contrast performance. This study assumes wavefront aberrations based on a finite element model of a simulated telescope with spacecraft structural dynamics. Wavefront residuals are then computed according to a model of the adaptive optics system that includes numerical propagation to simulate a realistic wavefront sensor and an analytical model of the temporal performance. An end-to-end numerical propagation model of ECLIPS is then used to estimate the residual starlight intensity distribution at the science detector. We show that the contrast performance depends strongly on the target star magnitude and the spatio-temporal distribution of wavefront errors from the telescope. In cases with significant vibration, we advocate for the use of laser metrology to mitigate high temporal frequency wavefront errors and increase the mission yield.

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“…29) is under construction at the University of Arizona. This testbed will serve as the primary platform for testing the CDEEP mission concept, as well as investigations into VVC technology and electric field conjugation focal plane wavefront sensing 85 . The highperformance and compact form factor are ideal for prototyping future high-contrast imaging instrumentation intended for spaceborne observatories.…”

Section: Long-slit Cross-dispersion Spectroscopy Formentioning

confidence: 99%

Advances in optical engineering for future telescopes

Kim¹,

Choi²,

Brendel³

et al. 2021

OEA

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Significant optical engineering advances at the University of Arizona are being made for design, fabrication, and construction of next generation astronomical telescopes. This summary review paper focuses on the technological advances in three key areas. First is the optical fabrication technique used for constructing next-generation telescope mirrors. Advances in ground-based telescope control and instrumentation comprise the second area of development. This includes active alignment of the laser truss-based Large Binocular Telescope (LBT) prime focus camera, the new MOBI-US modular cross-dispersion spectroscopy unit used at the prime focal plane of the LBT, and topological pupil segment optimization. Lastly, future space telescope concepts and enabling technologies are discussed. Among these, the Nautilus space observatory requires challenging alignment of segmented multi-order diffractive elements. The OASIS terahertz space telescope presents unique challenges for characterizing the inflatable primary mirror, and the Hyperion space telescope pushes the limits of high spectral resolution, far-UV spectroscopy. The Coronagraphic Debris and Exoplanet Exploring Pioneer (CDEEP) is a Small Satellite (SmallSat) mission concept for high-contrast imaging of circumstellar disks and exoplanets using vector vortex coronagraph. These advances in optical engineering technologies will help mankind to probe, explore, and understand the scientific beauty of our universe.

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The LUVOIR Extreme Coronagraph for Living Planetary Systems (ECLIPS) I: searching and characterizing exoplanetary gems

Cited by 20 publications

References 59 publications

Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

LUVOIR-ECLIPS closed-loop adaptive optics performance and contrast predictions

Advances in optical engineering for future telescopes

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