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The relativistically broadened Fe K$\alpha$ line, originating from theaccretion disc in a vicinity of a super massive black hole, is observed in onlyless than 50\% of type 1 Active Galactic Nuclei (AGN). In this study weinvestigate could this lack of detections be explained by the effects ofcertain parameters of the accretion disc and black hole, such as theinclination, the inner and outer radius of disc and emissivity index. In orderto determine how these parameters affect the Fe K $\alpha$ line shape, wesimulated about 60,000 Fe K $\alpha$ line profiles emitted from therelativistic disc.  Based on simulated line profiles, we conclude that the lack of the FeK$\alpha$ line detection in type 1 AGN could, be caused by the specificemitting disc parameters, but also by the limits in the spectral resolution andsensitivity of the X-ray detectors.

The shape of Fe K$\alpha$ line emitted from relativistic accretion disc around AGN black holes