The localized chemical pollution in NGC 5253 revisited: Results from deep echelle spectrophotometry

Abstract

We present echelle spectrophotometry of the blue compact dwarf galaxy (BCDG) NGC 5253. The data have been taken with the Very Large Telescope UVES echelle spectrograph in the 3100 to 10400 angstroms range. We have measured the intensities of a large number of permitted and forbidden emission lines in four zones of the central part of the galaxy. In particular, we detect faint C II and O II recombination lines (RLs). This is the first time that these lines are unambiguously detected in a dwarf starburst galaxy. The physical conditions of the ionized gas have been derived using a large number of different line intensity ratios. Chemical abundances of He, N, O, Ne, S, Cl, Ar, and Fe have been determined following the standard methods. In addition, C^{++} and O^{++} abundances have been derived from pure RLs. These abundances are larger than those obtained from collisionally excited lines, (CELs) (from 0.30 to 0.40 dex for C^{++} and from 0.19 to 0.28 dex for O^{++}). This result is consistent with a temperature fluctuations parameter (t^2) between 0.050 and 0.072. We confirm previous results that indicate the presence of a localized N enrichment in certain zones of the center of the galaxy. Moreover, our results also indicate a possible slight He overabundance in the same zones. The enrichment pattern agrees with that expected for the pollution by the ejecta of massive stars in the Wolf-Rayet (WR) phase. The amount of enriched material needed to produce the observed overabundance is consistent with the mass lost by the number of WR stars estimated in the starbursts. Finally, we discuss the possible origin of the difference between abundances derived from RLs and CELs in H II regions, finding that a recent hypothesis based on the delayed enrichment by SNe ejecta inclusions seems not to explain the observed features.