ner_tags: O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O B-CelestialObject O B-Instrument I-Instrument O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-ObservationalTechniques I-ObservationalTechniques I-ObservationalTechniques O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O B-CelestialObject O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Instrument I-Instrument O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O B-CelestialObject O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O B-Instrument I-Instrument O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: period for the outermost planet of 192 d, i.e. one third of the period found by Burke et al. (2014) . They reported planetary masses for the two giant objects of and . We secured five observations of KOI-1574 with SOPHIE HE. The data have a rms of 12 m s which is compatible with the uncertainties. The bisector and FWHM have rms of 44 m s and 38 m s, respectively. We fitted four circular orbits to the data fixing the orbital ephemeris to the transit ones. For KOI-1574.02, we choose the period of 572 days. We detect a hint of variation for the EGP at 114 days, with an amplitude of m s, and an upper limit of m s within the 99% confidence interval. For the other planets, we find upper limits at the 99% level on their amplitudes of m s, m s, and m s. Assuming a stellar host mass of ( Ofir et al. 2014 ), it gives a mass constraint for the EGP in our sample of ( at the 99% level). This value is fully compatible with the one derived by the transit timing analysis of Ofir et al. (2014) . For the other planet candidates, we find upper limits on the mass at the 99% level of , , and . Assuming that KOI-1574.02 orbits with a period of 192 d, as stated by Ofir et al. (2014) , does not change significantly our constraints on the mass of KOI-1574.01. For the other planets, the upper limits at 99% change to , , and . We conclude that none of these transiting candidates is an eclipsing brown dwarf or low-mass star eclipsing the target star. We confirm they have a mass within the planetary range. Appendix A.35: KOI-1645.01 The giant-planet candidate KOI-1645.01 was found by Burke et al. (2014) with an orbital period of 41 days. We observed it twice with SOPHIE HE and find a clear SB2. We fitted the cross-correlation function with a two-Gaussian profile to derive the RV of both stars. We call star A the one with the deepest line profile and star B the one with the shallowest line profile. The variation of both stars is anti-correlated, which gives a mass ratio of 87.6%. The star A exhibits a RV variation in anti-phase with the Kepler ephemeris, revealing that the secondary eclipse was detected in the light-curve. This candidate is not a transiting planet but a secondary-only EB. Appendix A.36: KOI-1783.01 A giant-planet candidate was found to transit the host star KOI-1783 with a period of 134d by Batalha et al. (2013) . We observed it twice with SOPHIE HE and find no significant RV variation. The bisector and FWHM variation are also compatible with their photon noise. By fitting a circular orbit with no drift at the transit ephemeris, we find an upper limit at the 99% level on the RV amplitude of m s. We derived the stellar atmospheric parameters that are reported in Table B.2 . We find a host mass of , a radius of , and an age of Gyr. Combining the two analyses, we derive an upper limit on the mass of this candidate of , within the 99% confidence interval. We can therefore exclude a star or brown dwarf eclipsing the target star, but we can not firmly