  (abridged)We present the observations of the pair of interacting galaxies
NGC6285/86 carried out with the 6m SAO RAS telescope by using 1D and 2D
spectroscopy. The observations of NGC6286 with a long-slit spectrograph (UAGS)
near the H-alpha line revealed the rotation of the gaseous disk around an axis
offset by 5''-7'' from the photometric center and a luminous gas at a distance
up to 9 kpc in a direction perpendicular to the galactic plane. Using a
multipupil fiber spectrograph (MPFS), we constructed the velocity fields of the
stellar and gaseous components in the central region of this galaxy, which
proved to be similar. The similar line-of-sight velocities of the pair and the
wide (5'x 5') field of view of the scanning Fabry-Perot interferometer (IFP)
allowed us to obtain images in the H-alpha and [NII]6583 emission lines and in
the continuum as well as to construct the line-of-sight velocity fields and to
map the distribution of the [NII]6583/H-alpha ratio for both galaxies
simultaneously. Based on these data, we studied the gas kinematics in the
galaxies, constructed their rotation curves, and estimated their masses. We
found no evidence of gas rotation around the major axis of NGC6286, which
argues against the assumption that this galaxy has a forming polar ring. The
IFP observations revealed an emission nebula around this galaxy with a
structure characteristic for superwind galaxies. The large [NII]6583/H-alpha
ratio, which suggests the collisional excitation of its emission, and the high
infrared luminosity are additional arguments for the hypothesis of a superwind
in the galaxy NGC 6286. A close encounter of the two galaxies was probably
responsible for the starburst and the bipolar outflow of hot gas from the
central region of the disk.
