A New Algorithm for Point-Spread Function Subtraction in High-Contrast Imaging: A Demonstration with Angular Differential Imaging

By D. Lafrèniere, C. Marois, R. Doyon, D. Nadeau, É. Artigau. 2007

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Direct imaging of exoplanets is limited by bright quasi-static speckles in the point-spread function (PSF) of the central star. This limitation can be reduced by subtraction of reference PSF images. We have developed an algorithm to construct an optimized reference PSF image from a set of reference images. This image is built as a linear combination of the reference images available, and the coefficients of the combination are optimized inside multiple subsections of the image independently to minimize the residual noise within each subsection. The algorithm developed can be used with many high-contrast imaging observing strategies relying on PSF subtraction, such as angular differential imaging (ADI), roll subtraction, spectral differential imaging, and reference star observations. The performance of the algorithm is demonstrated for ADI data. It is shown that for this type of data the new algorithm provides a gain in sensitivity by up to a factor of 3 at small separation over the algorithm previously used by Marois and colleagues.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ef72580b4caece9b75e090eb50531e4f79fcbfb7

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Citations in the corpus

THE VECTOR VORTEX CORONAGRAPH: LABORATORY RESULTS AND FIRST LIGHT AT PALOMAR OBSERVATORY (2009, methodology): “4 (left) shows our image of HR 7672 after postprocessing with the locally optimized combination of images algorithm (LOCI, Lafrenière et al. 2007), which is one of the most effective speckle subtraction techniques.”
Combining high-dispersion spectroscopy with high contrast imaging : Probing rocky planets around our nearest neighbors (2015, background): “…include Angular Differential Imaging (ADI; Marois et al. 2006), Spectral Differential Imaging (SDI; Racine et al. 1999), Locally Optimized Combinations of Images (LOCI; Lafrenière et al. 2007), and Principal Component Analysis (PCA; Amara & Quanz 2012, Soummer et al. 2012, Meshkat et al. 2014).”
Photometric characterization of exoplanets using angular and spectral differential imaging (2010, methodology): “…Imaging (SDI, Racine et al. 1999) or Angular Differential Imaging (ADI, Marois et al. 2006) to obtain data which will be analyzed using advanced methods such as Spectral Deconvolution (Sparks & Ford 2002) or Localy Optimized Combination of Images (LOCI, Lafrenière et al. 2007) for IRDIS data.”
Adaptive Optics for Astronomy (2012, methodology): “Although a few exoplanets have now been imaged directly, a number of surveys – e.g. Biller et al. (2007) (45 targets), Lafrenière et al. (2007a) (85 targets), and Kasper et al. (2007) (22 targets) – have failed to detect any planets down to limits of a few MJ .”
A YOUNG PROTOPLANET CANDIDATE EMBEDDED IN THE CIRCUMSTELLAR DISK OF HD 100546 (2013, methodology): “The PSF-subtraction was done using the principle component analysis based software package PynPoint (Amara & Quanz 2012), and the results were confirmed by using the LOCI algorithm (Lafrenière et al. 2007).”
ORBITAL MOTION OF HR 8799 b, c, d USING HUBBLE SPACE TELESCOPE DATA FROM 1998: CONSTRAINTS ON INCLINATION, ECCENTRICITY, AND STABILITY (2011, methodology): “A third parameter dr is used by Lafrenière et al. (2007b) to describe the width of the S−zone.”
The Gemini Deep Planet Survey (2007, methodology): “The subsections geometry and the algorithm parameters determined in Lafrenière et al. (2007) were used for all targets.”
CLOUDS AND CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HR8799b (2011, methodology): “Since the discovery of the HR8799 planetary system more broad-band observations have been published and improvements have been made in the LOCI (Lafrenière et al. 2007) and ADI algorithms (at least those used by this group).”
THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, methodology): “Based on a sample of 118 stars compiled from the surveys of Masciadri et al. (2005), Biller et al. (2007), and Lafrenière et al. (2007a), Nielsen & Close (2010) found that planets more massive than 4 MJup are found around <20% of FGKM stars in orbits between 22 and 507 AU, at 95% confidence.”
EXOPLANET ALBEDO SPECTRA AND COLORS AS A FUNCTION OF PLANET PHASE, SEPARATION, AND METALLICITY (2010, methodology): “…2002; Kasdin et al. 2003; Guyon et al. 2005; Trauger & Traub 2007; Mawet et al. 2009), external occulters (Cash 2006), and optical nullers (Wallace et al. 2000; Martin Levine et al. 2006), as well as post-processing algorithms such as those used by Marois et al. (2006) and Lafreniere et al. (2007).”
LkCa 15: A YOUNG EXOPLANET CAUGHT AT FORMATION? (2011, methodology): “Like the LOCI algorithm used to reduce AO direct imaging data (Lafrenière et al. 2007), finding an optimal linear combination of calibrators in this way tends to reduce the significance of a real companion in the data.”