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We present the results of our study of star-forming regions in the lenticular galaxy NGC 4324. During a complex analysis of multiwavelength observational data—the narrow-band emission-line images obtained with the 2.5-m telescope at the Caucasus Mountain Observatory of the Sternberg Astronomical Institute of the Moscow State University and the archival images in the broad photometric bands of the SDSS, GALEX and WISE space telescope surveys—we have detected young star-forming complexes (clumps) located in the inner ring of the lenticular galaxy NGC 4324 and established a regular pattern of their distribution along the ring, which, nevertheless, changes with time (with age of star-forming regions). We suggest several possible evolutionary paths of the lenticular galaxy NGC 4324, of which the swallowing of gas-rich satellites or giant clouds (the so-called minor merging) is the most probable one. [ABSTRACT FROM AUTHOR]

Abstract—Using the MaNGaL tunable-filter photometer at the 2.5-m telescope of the Caucasian Mountain Observatory of the Sternberg Astronomical Institute of Lomonosov Moscow State University, we studied star formation in an early-type gas-rich galaxy, which was until now considered to be elliptical,—NGC 5173. The gas has probably been accreted in the recent past by the galaxy from a direction inclined to its disk. Star formation that we observe now has led in the past 400 Myr to the formation of compact massive clusters with shock excitation of gas around them—a star formation behavior corresponding to what is usually observed in the interacting Antennae-like galaxies. In combination with the almost solar metallicity of the gas, this allows us to conclude that NGC 5173 has assimilate a very gas-rich companion with a mass of at least 10–20% of its own stellar mass. [ABSTRACT FROM AUTHOR]