Аннотация:For the galaxy NGC 1222 we obtained narrow-band images in the emission lines Hα, [NII]λ6583, and [OIII]λ5007 at the 2.5-meter telescope of the Caucasus Mountain Observatory of the Sternberg Astronomical Institute of the Moscow State University, which showed that the ionized gas is located in a limited domain of the central part of the main galaxy and in the satellite to the south-southwest of it. The regions of current star formation are located there, which ionize the gas. The long-slit spectra obtained by us at the 6-meter telescope BTA of the Special Astrophysical Observatory of the Russian Academy of Sciences in two position angles allowed us to draw line-of-sight velocity curves for various components of the ionized gas that revealed themselves in the emission, and as a result, to detect kinematic features in the sites of satellites intrusions, which confirm their accretion origin. A large number of emission lines in the spectra allowed us to apply several methods for estimating the oxygen abundance in the gas (i.e. the gas metallicity). As a result, we found differences in the metallicity of gas in the satellite at the south-southwest, in the regions of star formation in the central part of NGC 1222 and in the gas feeding them. Thus, inside of the previously acquired extensive low-metallicity gas disk of neutral hydrogen, more oxygen-enriched gas is detected, which appeared as a result of accretion from different sides (from the east and from the south-southwest) of two satellites, and the subsequent star formation induced in the sites of their intrusion.
