We present the detection and characterization of the two new transiting , close-in , giant extrasolar planets KOI-200 b and KOI-889 b . They were first identified by the Kepler  team as promising candidates from photometry of the Kepler  satellite , then we established their planetary nature thanks to the radial velocity follow-up jointly secured with the spectrographs SOPHIE and HARPS-N . Combined analyses of the whole datasets allow the two planetary systems to be characterized . The planet KOI-200 b has mass and radius of 0.68 \pm 0.09  M _ { \mathrm { Jup } }  and 1.32 \pm 0.14  R _ { \mathrm { Jup } } ; it orbits in 7.34 days a F8V host star with mass and radius of 1.40 ^ { +0.14 } _ { -0.11 }  \mathrm { M } _ { \odot }  and 1.51 \pm 0.14  \mathrm { R } _ { \odot } . KOI-889 b is a massive planet with mass and radius of 9.9 \pm 0.5  M _ { \mathrm { Jup } }  and 1.03 \pm 0.06  R _ { \mathrm { Jup } } ; it orbits in 8.88 days an active G8V star with a rotation period of 19.2 \pm 0.3  days , and mass and radius of 0.88 \pm 0.06  \mathrm { M } _ { \odot }  and 0.88 \pm 0.04  \mathrm { R } _ { \odot } . Both planets lie on eccentric orbits and are located just at the frontier between regimes where the tides can explain circularization and where tidal effects are negligible . The two planets are among the first ones detected and characterized thanks to observations secured with HARPS-N , the new spectrograph recently mounted at the Telescopio Nazionale Galileo . These results illustrate the benefits that could be obtained from joint studies using two spectrographs as SOPHIE and HARPS-N .