Linear and Bayesian Planet Detection Algorithms for the<i>Terrestrial Planet Finder</i>

Kasdin, N. Jeremy; Braems, Isabelle

doi:10.1086/505017

Cited by 30 publications

(41 citation statements)

References 8 publications

(16 reference statements)

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“…The computational requirements can, however, be very high. A Bayesian approach has been proposed in [14] as well. In this paper, the authors analyze the measurement and noise statistics and devise a second method, based on the estimation of observation time.…”

Section: Why Do We Need Another Algorithm?mentioning

confidence: 99%

“…This can be seen as a first attempt to design a system/algorithm that is optimized (in a given sense) for the task of interest. The remarkable result of [14] is that, for high background intensity, the point-spread function (PSF) matching filter is the optimal linear detector.…”

Section: Why Do We Need Another Algorithm?mentioning

confidence: 99%

“…Expanding the matrix products in Eq. (13) and simplifying, we can rewrite the loglikelihood ratio λ(g | r p ) as (14) ( 15) For a fixed r p and ḡ 0 (as in the SKE case), the first and third terms that appear in Eq. (15) between brackets do not vary with g; hence, they can be included in the constant against which λ(g | r p ) will be compared.…”

Section: Hotelling and Ideal Observers In Adaptive Opticsmentioning

confidence: 99%

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Application of the Hotelling and ideal observers to detection and localization of exoplanets

et al. 2007

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The ideal linear discriminant or Hotelling observer is widely used for detection tasks and imagequality assessment in medical imaging, but it has had little application in other imaging fields. We apply it to detection of planets outside of our solar system with long-exposure images obtained from ground-based or space-based telescopes. The statistical limitations in this problem include Poisson noise arising mainly from the host star, electronic noise in the image detector, randomness or uncertainty in the point-spread function (PSF) of the telescope, and possibly a random background. PSF randomness is reduced but not eliminated by the use of adaptive optics. We concentrate here on the effects of Poisson and electronic noise, but we also show how to extend the calculation to include a random PSF. For the case where the PSF is known exactly, we compare the Hotelling observer to other observers commonly used for planet detection; comparison is based on receiver operating characteristic (ROC) and localization ROC (LROC) curves.

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Section: Why Do We Need Another Algorithm?mentioning

confidence: 99%

Section: Why Do We Need Another Algorithm?mentioning

confidence: 99%

Section: Hotelling and Ideal Observers In Adaptive Opticsmentioning

confidence: 99%

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Application of the Hotelling and ideal observers to detection and localization of exoplanets

et al. 2007

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“…These can be generated based solely on statistical modeling as in Ref. 34, or can again be generated by actually processing simulated images.…”

Section: Postprocessingmentioning

confidence: 99%

WFIRST-AFTA coronagraph science yield modeling with EXOSIMS

Savransky

Garrett

2015

J. Astron. Telesc. Instrum. Syst

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Abstract. We present and discuss the design details of an extensible, modular, open-source software framework called EXOSIMS (Exoplanet Open-Source Imaging Mission Simulator), which creates end-to-end simulations of space-based exoplanet imaging missions. We motivate the development and baseline implementation of the component parts of this software with models of the wide-field infrared survey telescope-astrophysics focused telescope assets (WFIRST-AFTA) coronagraph and present initial results of mission simulations for various iterations of the WFIRST-AFTA coronagraph design. We present and discuss two sets of simulations. The first compares the science yield of completely different instruments in the form of early competing coronagraph designs for WFIRST-AFTA. The second set of simulations evaluates the effects of different operating assumptions, specifically the assumed postprocessing capabilities and telescope vibration levels. We discuss how these results can guide further instrument development and the expected evolution of science yields. © The Authors. Published by SPIE under a Creative CommonsAttribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requiresfull attribution of the original publication, including its DOI.

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“…16 In short, matched filtering consists in subtracting the background model from the images produced by the coronagraph and then cross-correlating the results with the Point Spread Function (PSF) of the telescope. To derive the signal-to-noise ratio (SNR) at each position, the matched-filtered images are then divided by the photon noise map at each position (see result in the SNR maps displayed in Fig.…”

Section: Planet Signal Extractionmentioning

confidence: 99%

Direct imaging of exoEarths embedded in clumpy debris disks

Defrère

Stark

Cahoy

et al. 2012

Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave

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The inner solar system, where the terrestrial planets formed and evolve, is populated by small grains of dust produced by collisions of asteroids and outgassing comets. At visible and infrared wavelengths, this dust cloud is in fact the most luminous component in the solar system after the Sun itself and the Earth may appear similar to a clump of zodiacal dust to an external observer. Hence, the presence of large amounts of dust in the habitable zone around nearby main-sequence stars is considered as a major hurdle toward the direct imaging of exoEarths with future dedicated space-based telescopes. In that context, we address in this paper the detectability of exoEarths embedded in structured debris disks with future space-based visible coronagraphs and mid-infrared interferometers. Using a collisional grooming algorithm, we produce models of dust clouds that simultaneously and self-consistently handle dust grain dynamics, including resonant interactions with planets, and grain-grain collisions. Considering various viewing geometries, we also derive limiting dust densities that can be tolerated around nearby main-sequence stars in order to ensure the characterization of exoEarths with future direct imaging missions.

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Linear and Bayesian Planet Detection Algorithms for theTerrestrial Planet Finder

Cited by 30 publications

References 8 publications

Application of the Hotelling and ideal observers to detection and localization of exoplanets

Application of the Hotelling and ideal observers to detection and localization of exoplanets

WFIRST-AFTA coronagraph science yield modeling with EXOSIMS

Direct imaging of exoEarths embedded in clumpy debris disks

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