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Complexities in the X‐ray spectrum of the nearby Seyfert 1.2 galaxy MCG–6‐30‐15 are commonly interpreted in terms of a broad iron line and the associated Compton reflection hump from the innermost relativistic regions of an accretion disc around a rapidly spinning black hole. However, an alternative model has recently been proposed in which these spectral features are caused entirely by complex (ionized and partial‐covering) absorption. By considering the fluorescent emission that must accompany photoelectric absorption, we show that the absorption‐dominated model overpredicts the 6.4 keV iron line flux unless the marginally Compton‐thick absorber responsible for the hard X‐ray hump satisfies very restrictive geometric constraints. In the absence of a specific model that both obeys these geometrical constraints and is physically plausible, the relativistic‐reflection model is favoured.

Constraints on the absorption‐dominated model for the X‐ray spectrum of MCG–6‐30‐15