We present our spectroscopic observations of the galaxy NGC 7468 performed at the 6-m Special Astrophysical Observatory telescope using the UAGS long-slit spectrograph, the multipupil fiber spectrograph MPFS, and the scanning Fabry-Perot interferometer (IF

4Shalyapina et al.:NGC 7468:a galaxy with an inner polar

disk Fig.2.NGC 7468:the UAGS line-of-sight velocity curves.

The three bright knots that correspond to condensa-

tions “a”,“b”,and “c”noted by Petrosyan et al.(1978)

are clearly seen in the central part of the image in the

green continuum (Fig.4c).Condensation “c”is brightest.

In the emission lines (Fig.4),condensation “c”is poorly

seen,while condensation “a”is most prominent.This char-

acteristic feature was noted by Petrosyan (1981).THE VELOCITY FIELDS OF THE IONIZED GAS AND STARS Figure 5a shows the large-scale velocity field for the emitting gas,as constructed from the IFP data,suggesting the rotation of the galaxy’s gaseous disk around its minor axis.However,a feature indicating the rotation of the gas around the galaxy’s major axis is clearly seen in the central part of the velocity field.Thus,the IFP data confirm the

presence of two kinematic subsystems of gas in this galaxy.If the gas is assumed to rotate in circular orbits,then the method of “tilted-rings”can be used (Begeman 1989;Moiseev and Mustsevoi 2000)to analyze the velocity field.The method allows us to determine the positions of the kinematic center and the kinematic axis (the direction of the maximum velocity gradient),to estimate the galaxy’s inclination,and to construct the rotation curve.As we see

from Fig.6b,the location of the kinematic axis changes

with increasing radius:P A dyn ≈120◦in the nuclear re-

gion (R ≤6′′)and P A dyn ≈180◦on the periphery.This

confirms the existence of two kinematic subsystems of gas.

The locations of the dynamic axes of the subsystems are

close to those estimated from long-slit spectra.The sub-

system associated with the central region is apparently the

inner disk (ring)rotating around the galaxy’s major axis.

The dynamic centers of the subsystems coincide,but are

displaced by approximately 3′′to the W of condensation

“a”.The heliocentric line-of-sight velocity of the galaxy