Two possible examples of the evolution in the proto–nuclear star cluster GN-z11, in the hypothesis that the AGB winds mixed with standard interstellar gas constitute the gas responsible for the high (N/O) abundances in the spectrum. The intra cluster medium exhibits the correct N/O, when polluted by the ejecta properly diluted of any of the intermediate mass AGB stars. The pink rectangle is the fiducial error box by Cameron et al. (2023) for GN-z11. In panel a, we assume that the 6 M_⊙ is the mass presently evolving, while in panel b we assume that the 4.5 M_⊙ is evolving, at the age of 430 Myr. The formation of the 1G is shifted back by 70 Myr (the evolution age of the 6 M_⊙) in panel a and by 130 Myr (the evolution age of the 4.5 M_⊙), respectively at ∼360 Myr or ∼300 Myr, as shown by the “ruler” drawn at the bottom. Asterisks denote the initial log(N/O) in the models, and colored squares represent the abundance in the ejecta. If we were to be witnessing the evolution of a larger (smaller) mass, the AGB abundances and the boxes would be all shifted to larger (smaller) age. The two lines at the bottom represent the time evolution of log(N/O) for the upper (full line) and lower (dashed) envelope of the chemical evolution models by Vincenzo et al. (2016).