Ionized gas in the NGC 3077 galaxy
  The nearby dwarf galaxy NGC 3077 is known for its peculiar morphology, which
includes numerous dust lanes and emission-line regions. The interstellar medium
in this galaxy is subject to several perturbing factors. These are primarily
the central starburst and tidal structures in the M 81 group. We present a
comprehensive study of the state of ionization, kinematics, and chemical
composition of ionized gas in NGC 3077, including both star-forming regions and
diffuse ionized gas (DIG) at the periphery. We study gas motions in the
H$\alpha$ line via high-resolution ($R\approx15\,000$) 3D spectroscopy with the
scanning Fabry-Perot interferometer installed into SCORPIO-2 instrument
attached to the 6-m telescope of the SAO RAS. Images in the main optical
emission lines were acquired with MaNGaL photometer with a tunable filter at
the 2.5-m telescope of the Caucasian Mountain Observatory of SAI MSU. We also
used SCORPIO-2 to perform long-slit spectroscopy of the galaxy with a
resolution of $R\approx1\,000$. Our estimate of the gas metallicity,
$Z=0.6Z_\odot$, is significantly lower than the earlier determination, but
agrees with the "luminosity--metallicity" dependence. Spatially resolved
diagnostic diagrams of the emission-line ratios do not show correlations
between the gas ionization state and its velocity dispersion, and this is most
likely due to strong ionization by young stars, whereas the contribution of
shocks to the excitation of emission lines is less important. We also studied
the locations of multicomponent H$\alpha$ profiles and provide arguments
suggesting that they are mostly associated with individual kinematic components
along the line of sight and not with expanding shells as it was believed
earlier. We also observe there a combination of wind outflow from star-forming
regions and accretion from interstellar gas clouds in the M 81 group.
