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(Abridged) The chemical behaviour of an ample sample of PNe in NGC6822 isanalyzed. Spectrophotometric data of 11 PNe and two H II regions were obtainedwith the OSIRIS spectrograph attached to the Gran Telescopio Canarias. Data forother 13 PNe and three H II regions were retrieved from the literature.Physical conditions and chemical abundances of O, N, Ne, Ar and S were derivedfor 19 PNe and 4 H II regions. Abundances in the PNe sample are widelydistributed showing 12+log(O/H) from 7.4 to 8.2 and 12+log(Ar/H) from 4.97 to5.80. Two groups of PNe can be differentiated: one old, with low metallicity(12+log(O/H)<8.0 and 12+log(Ar/H)<5.7) and another younger with metallicitiessimilar to the values of H II regions. The old objects are distributed in alarger volume than the young ones. An important fraction of PNe (>30%) wasfound to be highly N-rich (Type I PNe). Such PNe occur at any metallicity. Inaddition, about 60% of the sample presents high ionization (He++/He >= 0.1),possessing a central star with effective temperature larger than 10^6 K.Possible biases in the sample are discussed. From comparison with stellarevolution models by A. Karakas's group of the observed N/O abundance ratios,our PNe should have had initial masses lower than 4 M_sun, although if thecomparison is made with Ne vs. O abundances, the initial masses should havebeen lower than 2 M_sun. It appears that these models of stars of 2-3 M_sun areproducing too much 22Ne in the stellar surface at the end of the AGB. On theother hand, the comparison with another set of stellar evolution models by P.Ventura's group with a different treatment of convection and on the assumptionsconcerning the overshoot of the convective core during the core H-burningphase, provided a reasonable agreement between N/O and Ne/H observed andpredicted ratios if initial masses of more massive stars are of about 4 M_sun.

The PNe and H II regions in NGC 6822 revisited. Clues to AGB nucleosynthesis