Transiting planet search in the Kepler pipeline

被引：187

作者：

Jenkins, Jon M. ^{[1
]}

Chandrasekara, Hema ^{[1
,2
]}

McCauliff, Sean D. ^{[3
]}

Caldwell, Douglas A. ^{[1
]}

Tenenbaum, Peter ^{[1
]}

Li, Jie ^{[1
]}

Klaus, Todd C. ^{[3
]}

Cote, Miles T. ^{[4
]}

Middour, Christopher ^{[3
]}

机构：

[1] NASA, Ames Res Ctr, SETI Inst, M-S 244-30, Stanford, CA 94305 USA

[2] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA

[3] NASA, Ames Res Ctr, Orbital Sci Corp, Stanford, CA 94305 USA

[4] NASA, Ames Res Ctr, Stanford, CA 94305 USA

来源：

SOFTWARE AND CYBERINFRASTRUCTURE FOR ASTRONOMY | 2010年 / 7740卷

关键词：

Kepler Mission; exoplanet; transit; detection algorithm;

D O I：

10.1117/12.856764

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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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页数：11

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