Stars and ionized gas in S0 galaxy NGC 7743: an inclined large-scale
  gaseous disk
  We used deep long-slit spectra and integral-field spectral data to study the
stars and ionized gas kinematics and stellar population properties in the
lenticular barred galaxy NGC 7743. We have shown that ionized gas at the
distances larger than 1.5 kpc from the nucleus settles in the disk which is
significantly inclined to the stellar disk of the galaxy. Making different
assumptions about the geometry of the disks and involving different sets of
emission lines into the fitting, under the assumption of thin flat disk
circular rotation, we obtain the full possible range of angle between the disks
to be 34+/-9 or 77+/-9 deg. The most probable origin of the inclined disk is
the external gas accretion from a satellite, orbiting the host galaxy with a
corresponding angular momentum direction. The published data on the HI
distribution around NGC 7743 suggest that the galaxy has a gas-rich
environment. The emission-line ratio diagrams imply the domination of shock
waves in the ionization state of the gaseous disk, whereas the contribution of
photoionization by recent star formation seems to be negligible. In some parts
of the disk a difference between the velocities of the gas emitting in the
forbidden lines and in the Balmer lines is detected. It may be caused by the
fact that the inclined disk is mainly shock-excited, whereas some fraction of
the Balmer-line emission is produced by a small amount of gas excited by young
stars in the main stellar disk of NGC 7743. In the circumnuclear region (R< 200
pc) some evidences of the AGN jet interaction with an ambient interstellar
medium were found.
