Stellar yields (in solar masses) of ¹⁴N ejected by winds during evolution (left panel, computed as in Eq. (1)) and integrated above the mass coordinate of the CO core at the last computed stage of stellar evolution (right panel, computed as in Eq. (2)) for all models with initial mass M_ini ≥ 9M_⊙ at different metallicities (Z = 0 (Pop III, blue), Z = 10⁻⁵ (this paper, green), Z = 0.0004 (I Zw 18, yellow), Z = 0.006 (LMC, pink), Z = 0.014 (solar, purple)). Because some models yield less ¹⁴N than they contain on the ZAMS, the yield can be negative. This is indicated on the figure by the separation in the vertical axes, the dash-dotted line, and the arrows showing ‘Positive’ and ‘Negative’. The vertical axes are in different logarithmic scales. Solid lines: Non-rotating models. Dotted lines: Rotating models.