Wilms et al. (2001)  recently presented and discussed an extremely broad and red-shifted iron K&alpha; line, detected in the June 11-12, 2000, 100 ksec XMM-Newton observation of MCG-6-30-15. The line profile is extremely broad and redshifted, indicating that a large fraction of the emission comes from r<6r_g, and that the disc emissivity law is very steep.
If a simple powerlaw is used for the emissivity, the best-fit powerlaw index is ß ~   4, i.e. the dependence on radius is much steeper than usual in Seyfert galaxies (Nandra et al., 1997).
In this contribution we show that this emissivity, as well as the observed strong line Equivalent Width (EW ~  300 eV) and the amount of Compton reflection (R >> 1), may be reproduced by a model in which the primary X-ray source - located on the BH symmetry axis at a height h ~   a few r_g  (the gravitational radius) - illuminates the disc. This is the so called lamp-post picture (cp. Martocchia & Matt, 1996, Petrucci & Henry, 1997, Bao et al., 1998, Reynolds et al., 1999, Dabrowsky & Lasenby, 2001). It can be considered a phenomenological scheme appropriate for
models like those by Henry & Petrucci (1997) or Agol & Krolik (2001).

Further details can be found in: Martocchia, Matt & Karas (2001).