High-quality spectrophotometry of the planetary nebula in the Fornax dSph

Abstract

We present results of NTT spectroscopy of the one known planetary nebula (PN) in the dwarf spheroidal galaxy Fornax, a gas-deficient Local Group galaxy that stopped its star formation activity a few hundred million years ago. We detected the [O III] λ4363 line with a signal-to-noise ratio of ∼22. For the first time we detected the weak [SII] λλ6717,6731 lines (I(6717+6731) ≈ 0.01 1(Hβ)), determined the electron number density (Ne(SII) = 750 cm-3), and calculated O, N, Ne, Ar, S, Cl, Fe, He and C abundances. The abundance analysis presented here is based on the direct calculation of the electron temperature Te and yields an oxygen abundance of 12+log(O/H) = 8.28 ± 0.02. The analysis of the O, Ne, Ar and S abundances shows that the original ISM oxygen abundance was 0.27 ± 0.10 dex lower and that third-dredge-up self-pollution in oxygen took place. The blue spectrum shows weak Wolf-Rayet features, and the progenitor star is classified as a weak emission-line star. Four of the five PNe in dwarf spheroidal galaxies are now known to show WR wind features. Overall, the metallicity of the progenitor of the PN fits in well with stellar spectroscopic abundances derived in previous studies as well as with the stellar age-metallicity relation of Fornax. © ESO 2007.