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

2Shalyapina et al.:NGC7468:a galaxy with an inner polar disk

Fig.1.Image of the galaxy NGC7468obtained with the

6m telescope through afilter centered atλ6622˚A;the

UAGS slit locations and the MPFSfield during observa-

tions are shown.

interaction is believed to be the most probable cause of

the polar-ring formation and because she failed tofind

another suitable candidate that would confirm the inter-

action.Meanwhile,Taylor et al.(1993)pointed out that

there is a faint galaxy4.′6(45.5kpc)north of NGC7468

that the authors believe to be a possible companion of

NGC7468.The currently available information is clearly

insufficient to determine whether NGC7468belongs to

PRGs.The velocityfield of the galaxy should be stud-

ied with a high spatial resolution.This paper presents the

results of such a study based on optical spectroscopy.

OBSER V ATIONS AND DATA REDUCTION

We performed our spectroscopic observations of the

galaxy NGC7468at the prime focus of the6-m Special

Astrophysical Observatory(SAO)telescope with the long-

slit spectrograph(UAGS),the multipupilfiber spectro-

graph(MPFS)(Afanasiev et al.2001),and the scanning

Fabry-Perot interferometer(IFP)(see Moiseev(2002)and

the SAO WWW-site1).The table1gives a log of obser-

vations.

The reduction technique that we used was described

previously(Shalyapina et al.(2004).

The long-slit spectra were taken near the Hαline(see

the table1).The Hαand[SII]λλ6716,6730˚A emission

lines proved to be brightest in the spectra;in addition,

the[NII]λλ6548,6583˚A,HeIλ6678˚A lines were observed.

The line-of-sight velocity curves were constructed from all

lines.The accuracy of these measurements is±10km s−1.

The central region of the galaxy was observed with

the MPFS in the green spectral range.This range includes

metal absorption lines(MgIλ5175˚A,FeIλ5229˚A,FeI+CaI

λ5270˚A,etc.)and the Hβand[OIII]λλ4959,5007˚A emis-