Notes. The first group of 5 planets are the targets for which results were presented previously. The second group of 19 planets are the targets of this work. For each planet, Col. 6 provides the mean transit detection threshold (in ppm and [R_⊕]), as inferred from injection of transit models in the data (see Sect. 6 for details). Columns 7 and 8 give the theoretical radii corresponding, respectively, to a pure-iron and Earth-like compositions. Columns 9 and 10 present the a priori (geometric) and a posteriori (after observation) transit probabilities for the planet. ^(a) Not Applicable: for HD 13808 b and HD 115617 b (61 Vir b), our observations did not constrain the (non-)transiting configuration, while for HD 75732 e (55 Cnc e), HD 97658 b, and HD 219134 b, a transit was firmly detected in the data.

Reference. ⁽¹⁾ Gillon et al. (2010); ⁽²⁾ Bonfils et al. (2011); ⁽³⁾ Demory et al. (2011); ⁽⁴⁾ Gillon et al. (2012a); ⁽⁵⁾ Van Grootel et al. (2014); ⁽⁶⁾ Motalebi et al. (2015); ⁽⁷⁾ this work.