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Context: A planetary nebula (PN) candidate was discovered during FORS imagingof the Local Group dwarf galaxy Phoenix. Aims: Use this PN to complementabundances from red-giant stars. Methods: FORS spectroscopy was used to confirmthe PN classification. Empirical methods and photoionization modeling were usedto derive elemental abundances from the emission line fluxes and tocharacterize the central star. Results: For the elements deemed most reliablefor measuring the metallicity of the interstellar medium (ISM) from which thePN formed, [O/H] ~ -0.46 and [Ar/H] ~ -1.03. [O/H] has lower measurement errorsbut greater uncertainties due to the unresolved issue of oxygen enrichment inthe PN precursor star. Conclusions: Earlier than 2 Gyr ago (the lower limit ofthe derived age for the central star) the ISM had Z = 0.002--0.008, a rangeslightly more metal-rich than the one provided by stars. Comparing ourPN-to-stellar values to surveys for other dwarf Local Group galaxies, Phoenixappears as an outlier.

VLT/FORS1 spectrophotometry of the first planetary nebula discovered in the Phoenix dwarf galaxy