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Transiting planet search in the Kepler pipeline

Identifieur interne : 000A36 ( Main/Exploration ); précédent : 000A35; suivant : 000A37

Transiting planet search in the Kepler pipeline

Auteurs : Jon M. Jenkins [États-Unis] ; Hema Chandrasekaran [États-Unis] ; Sean D. Mccaulif [États-Unis] ; Douglas A. Caldwell [États-Unis] ; Peter Tenenbaum [États-Unis] ; JIE LI [États-Unis] ; Todd C. Klaus [États-Unis] ; Miles T. Cote [États-Unis] ; Christopher Middour [États-Unis]

Source :

RBID : Pascal:11-0006809

Descripteurs français

English descriptors

Abstract

The Kepler Mission simultaneously measures the brightness of more than 160,000 stars every 29.4 minutes over a 3.5-year mission to search for transiting planets. Detecting transits is a signal-detection problem where the signal of interest is a periodic pulse train and the predominant noise source is non-white, non-stationary (1/f) type process of stellar variability. Many stars also exhibit coherent or quasi-coherent oscillations. The detection algorithm first identifies and removes strong oscillations followed by an adaptive, wavelet-based matched filter. We discuss how we obtain super-resolution detection statistics and the effectiveness of the algorithm for Kepler flight data.


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Le document en format XML

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<div type="abstract" xml:lang="en">The Kepler Mission simultaneously measures the brightness of more than 160,000 stars every 29.4 minutes over a 3.5-year mission to search for transiting planets. Detecting transits is a signal-detection problem where the signal of interest is a periodic pulse train and the predominant noise source is non-white, non-stationary (1/f) type process of stellar variability. Many stars also exhibit coherent or quasi-coherent oscillations. The detection algorithm first identifies and removes strong oscillations followed by an adaptive, wavelet-based matched filter. We discuss how we obtain super-resolution detection statistics and the effectiveness of the algorithm for Kepler flight data.</div>
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