Volume 567, July 2014
|Number of page(s)||13|
|Section||Planets and planetary systems|
|Published online||23 July 2014|
Radial velocity measurements.
IDs, coordinates and magnitudes.
Planet and star parameters.
Maps showing the regions where the F-test resulted in solutions not excluded to a level above 3σ with the multiple transiting system solution (solutions excluded above 3σ appear white in the plot). The different configurations explored are sketched at the left of each plot. The color scale is for the different q-ratios of the binary star or for the radii of the planets, and the color intensities are for different levels of exclusion (more intense meaning less excluded). The ordinate axis shows the distance modulus (). Bound, or closer to the observer, second stars are excluded with CRIRES spectra for spectral types later than M2.5V (Guenther et al. 2013). Regions labelled as “partially excluded by HARPS" are those in which a second CCF would have been detected in the HARPS data. In the case of rapidly rotating stars, this second CCF might have been unnoticed. In every case, second stars with masses above 1.7 M⊙ have been assumed to be undetectable in the CCFs, which explains the vertical cuts at this value. The upper left parts of the plots are typically excluded because the hypothetical system would produce eclipse depths below the observed values. The diagonal solid lines labelled with different J values are plotted to provide a direct comparison with the exclusion values from the NACO J-band images given by Guenther et al. (2013): a J = 17 star would have been detected at (and above) 0.18′′ from the primary, a J = 18 at 0.23′′, and a J = 19 at 0.58′′.
|Open with DEXTER|
© ESO, 2014
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