  We present an investigation of the structure of the emission line region in a
sample of 12 single-peaked Active Galactic Nuclei (AGNs). Using the high
resolution H-beta and H-alpha line profiles observed with the Isaac Newton
Telescope (La Palma) we study the substructure in the lines (such as shoulders
or bumps) which can indicate a disk or disk-like emission in Broad Line Regions
(BLRs). Applying Gaussian analysis we found that both kinds of emission
regions, BLR and NLR, are complex. In this sample the narrow [OIII] lines are
composites of two components; NLR1 which have random velocities from \sim 200
to 500 km/s and systematic velocities toward the blue from 20 to 350 km/s, and
NLR2 with smaller random velocities (\sim 100-200 km/s) and a redshift
corresponding to the cosmological one. The BLR also have complex structure and
we apply a two-component model assuming that the line wings originate in a very
broad line region (VBLR) and the line core in an intermediate line region
(ILR). The VBLR is assumed to be an accretion disk and the ILR a spherical
emission region.
  The model fits very well the H-alpha and H-beta line profiles of the AGNs.
