Chemical abundances of the PRGs UGC 7576 and UGC 9796 - I. Testing the formation scenario

Context. The study of both the chemical abundances of HII regions in polar ring galaxies and their implications for the evolutionary scenario of these systems has been a step forward both in tracing the formation history of the galaxy and giving hints toward the mechanisms at work during the building of a disk by cold accretion process. It is now important to establish whether such results are typical of the class of polar disk galaxies as a whole. Aims. The present work aims at checking the cold accretion of gas through a “cosmic filament” as a possible scenario for the formation of the polar structures in UGC 7576 and UGC 9796. If these form by cold accretion, we expect the HII regions abundances and metallicities to be lower than those of same-luminosity spiral disks, with values of Z ∼ 1/10 Z� , as predicted by cosmological simulations. Methods. We used deep long-slit spectra, obtained with DOLORES@TNG in the optical wavelengths, of the brightest HII regions associated with the polar structures to derive their chemical abundances and star formation rate. We used the empirical methods, based on the intensities of easily observable lines, to derive the oxygen abundance 12+ log(O/H) of both galaxies. Such values are compared with those typical of different morphological galaxy types of comparable luminosity.