  Using a time series of high-resolution spectra and high-quality multi-colour
photometry, we reconstruct surface maps of the primary component of the RS CVn
type rapidly rotating eclipsing binary, SV Cam (F9V + K4V). We measure a mass
ratio, q, of 0.641(2) using our highest quality spectra and obtain surface
brightness maps of the primary component, which exhibit predominantly
high-latitude spots located between 60-70-degree latitudes with a mean filling
factor of about 35%. This is also indicated by the R-band light curve
inversion, subjected to rigourous numerical tests. The spectral subtraction of
the H-alpha line reveals strong activity of the secondary component. The excess
H-alpha absorption detected near the secondary minimum hints to the presence of
cool material partially obscuring the primary star. The flux ratios of Ca II
IRT excess emission indicate that the contribution of chromospheric plage
regions associated with star-spots is dominant, even during the passage of the
filament-like absorption feature.
