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Fig. 1.

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Illustration depicting the massive Pop III enrichment scenario. From left to right: (1) The formation of a massive Pop III star via accretion which generally occurs during the pre-MS but some stars may undergo short accretion phases during MS. If the accretion rate is below the critical limit described in Nandal et al. (2023), the star migrates to blue. (2) The transition to red at the end of core helium burning leads to the formation of large convective zones and pulsational mass loss as shown by the red mesh. (3) The collapse of a MS may lead to additional mass ejected and the eventual formation of a black hole. (4) Further accretion of ejected material onto the black hole creates the conditions for allowing nitrogen absorption lines to appear, as in the case of GN-z11 and CEERS 1019.

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