Tracing the outflow kinematics in Type 2 Active Galactic Nuclei
  We have used the sample of 577 active galactic nuclei Type 1.8-2 spectra (z <
0.25), taken from Sloan Digital Sky Survey, to trace the influence of the
outflow kinematics to the profiles of different emission lines (Hbeta, [O III],
Halpha, [N II], [S II]). All considered lines were fitted with two Gaussian
components: one which fits the core of the line, and another which fits the
wings. We gave the procedure for decomposition of Halpha+[N II] wavelength
band, for the spectra where these lines overlap. The influence of the
gravitational/non-gravitational kinematics to the line components is
investigated by comparing the dispersions of the line components with stellar
velocity dispersion. We found that wing components of all considered emission
lines have pure non-gravitational kinematics, the core components are
consistent with gravitational kinematics for the Halpha, [N II] and [S II]
lines, while in the [O III] there is evidence for contribution from
non-gravitational kinematics. We adopted the wing components as proxy of the
outflow contribution and we investigated the outflow kinematics by analysing
the correlations between widths and between shifts of the wing components of
different lines. We found the strong correlations between shifts and between
wing component widths of all considered lines, with exception of the Hbeta wing
component width. These correlations indicate that outflow dynamics systemically
affects all emission lines in spectrum. However, it reflects with different
strength in their profiles, which is observed as different widths of the wing
components. The strongest outflow signature is observed in the [O III] lines,
which have the broadest wing components, weaker in Halpha and [N II], and the
weakest in [S II]. These results imply that considered lines arise in different
parts of an outflowing region.
