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Volume 559, November 2013
Article Number A83
Number of page(s) 20
Section Planets and planetary systems
Published online 20 November 2013

Online material

Appendix A: Observed RV, BVS, and measured detection limits

thumbnail Fig. A.1

From left to right: 1) RV time series. 2) (RV, BVS) diagramme. The slope of the (RV, BVS) correlation is indicated. In a few cases, the value is obviously impacted by a single deviating data point. 3) rms-based detection limits with a 99.8% probability (solid black curve) and a 68.2% probability (dotted curve), achievable limits with a perfect sampling (black solid straight line) and achievable limits if the signal was limited only by photon and instrumental noises and with a perfect temporal sampling (dotted straight lines). The vertical lines in the (period, detection limit) diagramme indicate the timespan for each star. 4) detection limits obtained with the LPA method. “r” indicates the factor of improvement between the LPA and rms-based detection limits.

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thumbnail Fig. B.1

First column: RV versus time of a simulated equatorial spot covering 1.5% of the visible surface and a temperature contrast of 1200 K, for a seen edge-on sun-like star and for five different values of vsini from the upper panels to the lower panels: 3 km s-1, 10 km s-1, 30 km s-1, 50 km s-1, 80 km s-1. Second column: same for the bissectors. Third column: BVS versus RV. Fourth column: BVS versus time.

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thumbnail Fig. B.2

Same as Fig. 10 for an inclination of 30 degrees (three first lines) and 5 degrees (three last lines), a colatitude (from the pole) of 30 degrees (except 5th line with a colatitude of 60 degrees), and vsini (from upper panels to lower panels) of 3, 10, 40, 10, 10, and 10 km s-1.

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© ESO, 2013

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