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We investigate constraints for the size and location of the X-ray source in1H 0707-495 determined from the shape of the relativistically smearedreflection from the accretion disc. We develop a new code to model an extendedX-ray source and we apply it to all archival XMM observations of 1H 0707-495.Contrary to Wilkins et al. we find that the relativistic reflection in thissource is not consistent with an extended uniform corona. Instead, we find thatthe X-ray source must be very compact, with the size of at most a gravitationalradius, and located at most at a few gravitational radii from the black holehorizon. A uniform extended corona does indeed produce an emissivity which islike a twice broken power law, but the inner emissivity is fixed by the sourcegeometry rather than being a free parameter. In 1H0707-495, reflection from theinner disc is much stronger than expected for a uniformly extended source.Including the effect of ionised absorption from a wind does not change thisconclusion, but including scattered emission (and more complex absorption) fromthe wind can dramatically change the reflection parameters.

Geometry of the X-ray source 1H 0707-495