Volume 492, Number 2, December III 2008
|Page(s)||617 - 620|
|Published online||27 October 2008|
The BAST algorithm for transit detection
Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrae 2, 12489 Berlin, Germany e-mail: Stefan.Renner@dlr.de
2 Zentrum für Astronomie und Astrophysik, Technische Universität, Hardenbergstr. 36, 10623 Berlin, Germany
3 Departament d'Astronomia i Meteorologia, Facultat de Física, Universitat de Barcelona, Barcelona, C/ Martí Franqués 1, 08028 Barcelona, Spain
Accepted: 26 September 2008
Context. The pioneer space mission for photometric exoplanet searches, CoRoT, steadily monitors about 12 000 stars in each of its fields of view. Transit detection algorithms are applied to derive promising planetary candidates, which are then followed-up with ground-based observations.
Aims. We present BAST (Berlin Automatic Search for Transits), a new algorithm for periodic transit detection, and test it on simulated CoRoT data.
Methods. BAST searches for box-shaped signals in normalized, filtered, variability-fitted, and unfolded light curves. A low-pass filter is applied to remove high-frequency signals, and linear fits to subsections of data are subtracted to remove the star's variability. A search for periodicity is then performed in transit events identified above a given detection threshold. Some criteria are defined to better separate planet candidates from binary stars.
Results. From the analysis of simulated CoRoT light curves, we show that the BAST detection performance is similar to that of the Box-fitting Least-Square (BLS) method if the signal-to-noise ratio is high. However, the BAST box search for transits computes 10 times faster than the BLS method. By adding periodic transits to simulated CoRoT data, we show that the minimum periodic depth detectable with BAST is a linearly increasing function of the noise level. For low-noise light curves, the detection limit corresponds to a transit depth d 0.01%, i.e. a planet of 1 Earth radius around a solar-type star.
Key words: stars: planetary systems / methods: data analysis / techniques: photometric / occultations
© ESO, 2008
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