  We present briefly the first results obtained by the application of the
KYNREFREV-reverberation model, which is ready for its use in XSPEC. This model
computes the time dependent reflection spectra of the disc as a response to a
flash of primary power-law radiation from a point source corona located on the
axis of the black-hole accretion disc. The assumptions of the model are:
central Kerr black hole, surrounded by a Keplerian, geometrically thin,
optically thick, ionised disc with the possibility of defining the radial
density profile and a stationary hot point-like patch of plasma located on the
system rotation axis and emitting isotropic power-law radiation (lamp-post
geometry). Full relativistic ray-tracing code in vacuum is used for photon
paths from the corona to the disc and to the observer and from the disc to the
observer. The ionisation of the disc is set for each radius according to the
amount of the incident primary flux and the density of the accretion disc. In
this paper we comment on some preliminary results obtained through the analysis
of X-ray reverberation time-lags from 1H 0707-495 and IRAS 13224-3809.
