Geometry of the X-ray source 1H0707–495

We present constraints for the size and location of the X-ray source in 1H0707–495 determined from the shape of the relativistically smeared reflection from the accretion disc, using a new model for an extended X-ray source. We apply it to all archival XMM observations of 1H0707–495. In contrast to earlier works we find that the relativistic reflection in this source is not consistent with an extended uniform corona. Instead, we find that the X-ray source must be very compact, with the size of at most a gravitational radius, and located at most at a few gravitational radii from the black hole horizon. A uniform extended corona does indeed produce an emissivity which is like a twice broken power law, but the inner emissivity is fixed by the source geometry rather than being a free parameter. In 1H0707–495, reflection from the inner disc is much stronger than expected for a uniformly extended source.