XMM-Newton observation of the Seyfert 1 galaxy Fairall 9

We report an X-ray observation of the Fairall 9 Seyfert 1 galaxy performed in July 2000 with the EPIC cameras and Reflection Grating Spectrometers (RG S) on board the XMM-Newton observatory. Above 2 keV, the high signal to noi se ratio of the EPIC spectra shows an emission line at 6.38 +/- 0.03 keV wi th a measured equivalent width of 120 eV. An absorption edge is also detect ed at 7.64(-0.36)(+0:21) in the source rest frame that has not been reporte d before. Spectral fitting of the measured spectra with reflection models i ndicates that these imprinted features are likely the result of partial rep rocessing of a primary X-ray continuum by optically thick material. The pos itions in energy of the emission line and absorption edge are consistent wi th Compton reflection models from material containing iron in states of ion ization lower than FeXVII. The Fe K emission line is narrow suggesting that the reflection process arises from material relatively far from a putative central black hole. The best fit models show that the reflected spectrum m ask a steeper intrinsic power law slope even at energies lower than 5 keV. The extrapolation of this primary continuum to energies lower than 2 keV re veals the presence of a soft excess component contributing to 14 +/- 6% of the overall flux in the 0.3-1.0 keV energy range. No evidence is found for a warm absorber in this low energy part of the spectrum. The analysis resul ts are discussed within the frame of recent accretion disc models in which X-rays from the primary continuum source heat up the upper layers of the di sc thus creating very hot, optically thin plasmas on top of cooler denser m aterial.