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tokens: the residuals from the planet fit, we obtain ( r , ρ) BIS = (−0.39, −0.33), and ( r , ρ) S-index = (−0.06, 0.38), which indicates no correlation among these quantities. These results, for the HARPS and CORALIE data, can be seen in Fig. 9 , with the activity indices listed in Tables A1 and A2 . We also performed the bisector analysis on K2-238, and found ( r , ρ) BIS = (0.40, 0.37), which would indicate no correlation between the BIS and the FEROS RVs. For the residuals we found ( r , ρ) BIS = (0.50, 0.36), also indicative of no strong correlation. The results are shown in Fig. 10 , and listed in Table A3 . We did not include the S-index due to the low S/N spectra obtained with FEROS, which prohibited us from measuring them reliably. Figure 10. Correlations between the RVs (top panel) and the residuals from the planetary fit (bottom panel), with the BIS from FEROS for K2-238. The colours represent the orbital phase of the RV and residuals. r and ρ are the Pearson and Spearman correlation coefficients, respectively. 3.5 Planet scenario validation In order to confirm the planetary nature of our photometric and spectroscopic measurements, we performed a blend analysis using the algorithms described in Hartman et al. ( 2011a , b ), which model the observations taking into account the possibility that they could be generated by either a planet, stellar companions physically associated with our target star or by various blend scenarios, including blended eclipsing binary and hierarchical triple systems. K2-237 b is confirmed to be a planet based solely on the photometry; it is practically impossible for the best-fitting blend scenarios to fit the observed photometry in any of the cases consistent with the spectroscopic information. For K2-238 b , the planetary interpretation is also favoured by the data: although there is a detected close-by companion in the Lick 3 m Adaptive Optics (AO) data, the light curve is not consistent with the transit/eclipses arising from the neighbour, as all the simulated light-curve signatures imply J − K colours much less than the observed J − K = 0.631 ± 0.043. Considering that the brighter source could still itself be a blend, we can reject all the blend scenarios at 2.5σ confidence based on the photometry. However, none of them are able to produce the observed 100 m s −1 sinusoidal RV variation. The best-fitting blend scenarios to the photometry also yield large bisector span variations in excess of 1 km s −1 , which are clearly ruled out by our measurements (see Fig. 10 ). We consider thus both planets to be statistically validated given our photometric and spectroscopic measurements. 3.6 Searching for additional signals in the photometry We search for additional signals in our K2 light curves, produced by other companions, orbital phase variations, or secondary eclipses by performing a Box-fitting Least-Squares periodogram (BLS, Kovács, Zucker Mazeh 2002 ) on the light curves, with the transits of the detected