Context : The star HD 52265 is a G0V metal-rich exoplanet-host star observed in the seismology field of the CoRoT space telescope from November 2008 to March 2009 . The satellite collected 117 days of high-precision photometric data on this star , showing that it presents solar-like oscillations . HD 52265 was also observed in spectroscopy with the Narval spectrograph at the same epoch . Aims : We characterise HD 52265 using both spectroscopic and seismic data . Methods : The fundamental stellar parameters of HD 52265 were derived with the semi-automatic software VWA , and the projected rotational velocity was estimated by fitting synthetic profiles to isolated lines in the observed spectrum . The parameters of the observed p modes were determined with a maximum-likelihood estimation . We performed a global fit of the oscillation spectrum , over about ten radial orders , for degrees l = 0 to 2 . We also derived the properties of the granulation , and analysed a signature of the rotation induced by the photospheric magnetic activity . Results : Precise determinations of fundamental parameters have been obtained : T _ { \mathrm { eff } } = 6100 \pm 60 \mathrm { K } , \log g = 4.35 \pm 0.09 , \mathrm { [ M / H ] } = 0.19 \pm 0.05 , as well as v \sin i = 3.6 ^ { +0.3 } _ { -1.0 } \mathrm { km s ^ { -1 } } . We have measured a mean rotation period P _ { \mathrm { rot } } = 12.3 \pm 0.15 days , and find a signature of differential rotation . The frequencies of 31 modes are reported in the range 1500–2550 \mathrm { \mu Hz } . The large separation exhibits a clear modulation around the mean value \overline { \Delta \nu } = 98.3 \pm 0.1 \mathrm { \mu Hz } . Mode widths vary with frequency along an S-shape with a clear local maximum around 1800 \mathrm { \mu Hz } . We deduce lifetimes ranging between 0.5 and 3 days for these modes . Finally , we find a maximal bolometric amplitude of about 3.96 \pm 0.24 ppm for radial modes . Conclusions :