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Accretion models predict that fluorescence lines broadened by relativisticeffects should arise from reflection of X-ray emission onto the inner region ofthe accretion disc surrounding the central black hole of active galactic nuclei(AGN). The theory behind the origin of relativistic lines is well established,and observational evidence from a moderate number of sources seems to supportthe existence of these lines. The aim of this work is to establish the fractionof AGN with relativistic Fe Kalpha lines, and study possible correlations withsource physical properties. An XMM-Newton collection of 149 radio-quiet Type 1AGN has been systematically and uniformly analyzed in order to search forsignificant evidence of a relativistically broadened Fe Kalpha line. To enablestatistical studies, an almost complete, flux-limited subsample of 31 sourceshas been defined. The 2-10 keV spectra of the FERO sources have been comparedwith a complex model including most of the physical components observed in theX-ray spectra of Seyfert galaxies: a power law primary continuum modified bynon-relativistic Compton reflection and warm absorption, plus a series ofnarrow Fe line reflection features. The observed fraction of sources in theflux-limited sample that show significant evidence of a relativistic Fe Kalphaline is 36%. The average line Equivalent Width (EW) is of the order of 100 eV,while the average disc inclination angle is 28+/-5 deg and the averagepower-law index of the radial disc emissivity law is 2.4+/-0.4. The spin valueis well constrained only in 2 cases (MCG-6-30-15 and MRK509), and in the restof the cases, whenever a constraint can be placed, it always implies therejection of the static black hole solution. The Fe Kalpha line EW does notcorrelate with disc parameters or with system physical properties, such asblack hole mass, accretion rate and hard X-ray luminosity.

FERO: Finding Extreme Relativistic Objects. I. Statistics of Relativistic Fe Kalpha lines in Radio-Quiet Type 1 AGN