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The nearby dwarf galaxy NGC 3077 is known for its peculiar morphology, whichincludes numerous dust lanes and emission-line regions. The interstellar mediumin this galaxy is subject to several perturbing factors. These are primarilythe central starburst and tidal structures in the M 81 group. We present acomprehensive study of the state of ionization, kinematics, and chemicalcomposition of ionized gas in NGC 3077, including both star-forming regions anddiffuse ionized gas (DIG) at the periphery. We study gas motions in theH$\alpha$ line via high-resolution ($R\approx15\,000$) 3D spectroscopy with thescanning Fabry-Perot interferometer installed into SCORPIO-2 instrumentattached to the 6-m telescope of the SAO RAS. Images in the main opticalemission lines were acquired with MaNGaL photometer with a tunable filter atthe 2.5-m telescope of the Caucasian Mountain Observatory of SAI MSU. We alsoused SCORPIO-2 to perform long-slit spectroscopy of the galaxy with aresolution of $R\approx1\,000$. Our estimate of the gas metallicity,$Z=0.6Z_\odot$, is significantly lower than the earlier determination, butagrees with the "luminosity--metallicity" dependence. Spatially resolveddiagnostic diagrams of the emission-line ratios do not show correlationsbetween the gas ionization state and its velocity dispersion, and this is mostlikely due to strong ionization by young stars, whereas the contribution ofshocks to the excitation of emission lines is less important. We also studiedthe locations of multicomponent H$\alpha$ profiles and provide argumentssuggesting that they are mostly associated with individual kinematic componentsalong the line of sight and not with expanding shells as it was believedearlier. We also observe there a combination of wind outflow from star-formingregions and accretion from interstellar gas clouds in the M 81 group.

Ionized gas in the NGC 3077 galaxy