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Context. The study of abundances in the nucleus of active galaxies allows usto investigate the evolution of abundance by comparing local and higherredshift galaxies. However, the methods used so far have substantial drawbacksor rather large uncertainties. Some of the measurements are at odds with theinitial mass function derived from the older stellar population of localelliptical galaxies. Aims. We determine accurate and reliable abundances of C,N, Ne, and Fe relative to O from the narrow absorption lines observed in theX-ray spectra of Mrk 509. Methods. We use the stacked 600 ks XMM-Newton RGS and180 ks Chandra LETGS spectra. Thanks to simultaneous observations with INTEGRALand the optical monitor on-board XMM-Newton for the RGS observations andHST-COS and Swift for the LETGS observations, we have an individual spectralenergy distribution for each dataset. Owing to the excellent quality of the RGSspectrum, the ionisation structure of the absorbing gas is well constrained,allowing for a reliable abundance determination using ions over the wholeobserved range of ionisation parameters. Results. We find that the relativeabundances are consistent with the proto-solar abundance ratios: C/O =1.19$\pm$0.08, N/O = 0.98$\pm$0.08, Ne/O = 1.11$\pm$0.10, Mg/O = 0.68$\pm$0.16,Si/O = 1.3$\pm$0.6, Ca/O = 0.89$\pm$0.25, and Fe/O = 0.85$\pm$0.06, with theexception of S, which is slightly under-abundant, S/O = 0.57$\pm$0.14. Ourresults, and their implications, are discussed and compared to the resultsobtained using other techniques to derive abundances in galaxies.

Multiwavelength campaign on Mrk 509 VII. Relative abundances of the warm absorber