CyberinfraV1, Main, Exploration, bibRecord, 000B47

An algorithm for the fitting of planet models to Kepler light curves

Identifieur interne : 000B47 ( Main/Exploration ); précédent : 000B46; suivant : 000B48

An algorithm for the fitting of planet models to Kepler light curves

Auteurs : Peter Tenenbaum [États-Unis] ; Stephen T. Bryson [États-Unis] ; Hema Chandrasekaran [États-Unis] ; JIE LI [États-Unis] ; Elisa Quintana [États-Unis] ; Joseph D. Twicken [États-Unis] ; Jon M. Jenkins [États-Unis]

Source :

Proceedings of SPIE, the International Society for Optical Engineering [ 0277-786X ] ; 2010.

RBID : Pascal:11-0006802

Descripteurs français

Pascal (Inist)
- Semence, Système temporisé, Processus itératif, Centre gravité, Soustraction, Modélisation, Ajustement modèle, Transformation ondelette, Autocohérence, Variabilité, Approche probabiliste, Analyse statistique, ..
Wicri :
- topic : Semence.

English descriptors

KwdEn :
- Center of mass, Iterative process, Model matching, Modeling, Probabilistic approach, Seed, Self consistency, Statistical analysis, Subtraction, Timed system, Variability, Wavelet transformation.

Abstract

We describe an algorithm which fits model planetary system parameters to light curves from Kepler Mission target stars. The algorithm begins by producing an initial model of the system which is used to seed the fit, with particular emphasis on obtaining good transit timing parameters. An attempt is then made to determine whether the observed transits are more likely due to a planet or an eclipsing binary. In the event that the transits are consistent with a transiting planet, an iterative fitting process is initiated: a wavelet-based whitening filter is used to eliminate stellar variations on timescales long compared to a transit; a robust nonlinear fitter operating on the whitened light curve produces a new model of the system; and the procedure iterates until convergence upon a self-consistent whitening filter and planet model. The fitted transits are removed from the light curve and a search for additional planet candidates is performed upon the residual light curve. The fitted models are used in additional tests which identify false positive planet detections: multiple planet candidates with near-identical fitted periods are far more likely to be an eclipsing binary, for example, while target stars in which the model light curve is correlated with the star centroid position may indicate a background eclipsing binary, and subtraction of all model planet candidates yields a light curve of pure noise and stellar variability, which can be used to study the probability that the planet candidates result from statistical fluctuations in the data.

Affiliations:

Links toward previous steps (curation, corpus...)

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Le document en format XML

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<front><div type="abstract" xml:lang="en">We describe an algorithm which fits model planetary system parameters to light curves from Kepler Mission target stars. The algorithm begins by producing an initial model of the system which is used to seed the fit, with particular emphasis on obtaining good transit timing parameters. An attempt is then made to determine whether the observed transits are more likely due to a planet or an eclipsing binary. In the event that the transits are consistent with a transiting planet, an iterative fitting process is initiated: a wavelet-based whitening filter is used to eliminate stellar variations on timescales long compared to a transit; a robust nonlinear fitter operating on the whitened light curve produces a new model of the system; and the procedure iterates until convergence upon a self-consistent whitening filter and planet model. The fitted transits are removed from the light curve and a search for additional planet candidates is performed upon the residual light curve. The fitted models are used in additional tests which identify false positive planet detections: multiple planet candidates with near-identical fitted periods are far more likely to be an eclipsing binary, for example, while target stars in which the model light curve is correlated with the star centroid position may indicate a background eclipsing binary, and subtraction of all model planet candidates yields a light curve of pure noise and stellar variability, which can be used to study the probability that the planet candidates result from statistical fluctuations in the data.</div>
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An algorithm for the fitting of planet models to Kepler light curves

An algorithm for the fitting of planet models to Kepler light curves

Source :

Descripteurs français

English descriptors

Abstract

Links toward previous steps (curation, corpus...)

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri