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We investigate the global properties of the radiation emitted by theaccretion disk around Kerr black holes. Using the Kerr blackbody (KERRBB)numerical model, we build an analytic approximation of the disk emissionfeatures focusing on the pattern of the produced radiation as a function of theblack hole spin, mass, accretion rate and viewing angle. The assumption ofhaving a geometrically thin disk limits our analysis to systems emitting below~0.3 of the Eddington luminosity. We apply this analytical model to fourblazars (whose jets are pointing at us) at high redshift that show clearsignatures of disk emission. For them, we derive the black hole masses as afunction of spin. If these jetted sources are powered by the black holerotation, they must have high spin values, further constraining their masses.

How to constrain mass and spin of supermassive black holes through their disk emission