  We present the detection and characterization of the transiting warm Jupiter
KOI-12b, first identified with Kepler with an orbital period of 17.86 days. We
combine the analysis of Kepler photometry with Doppler spectroscopy and
line-profile tomography of time-series spectra obtained with the SOPHIE
spectrograph to establish its planetary nature and derive its properties. To
derive reliable estimates for the uncertainties on the tomographic model
parameters, we devised an empirical method to calculate statistically
independent error bars on the time-series spectra. KOI-12b has a radius of
1.43$\pm$0.13$ R_\mathrm{Jup}$ and a 3$\sigma$ upper mass limit of
10$M_\mathrm{Jup}$. It orbits a fast-rotating star ($v$sin$i_{\star}$ =
60.0$\pm$0.9 km s$^{-1}$) with mass and radius of 1.45$\pm$0.09
$M_\mathrm{Sun}$ and 1.63$\pm$0.15 $R_\mathrm{Sun}$, located at 426$\pm$40 pc
from the Earth. Doppler tomography allowed a higher precision on the obliquity
to be reached by comparison with the analysis of the Rossiter-McLaughlin radial
velocity anomaly, and we found that KOI-12b lies on a prograde, slightly
misaligned orbit with a low sky-projected obliquity $\lambda$ =
12.6$\stackrel{+3.0}{_{-2.9}}^\circ$. The properties of this planetary system,
with a 11.4 magnitude host-star, make of KOI-12b a precious target for future
atmospheric characterization.
