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Low metallicity stars give rise to unique spectacular transients and are ofimmense interest for understanding stellar evolution. Their importance has onlygrown further with the recent detections of mergers of stellar mass black holesthat likely originate mainly from low metallicity progenitor systems. Moreover,the formation of low metallicity stars is intricately linked to galaxyevolution, in particular to early enrichment and to later accretion and mixingof lower metallicity gas. Because low metallicity stars are difficult toobserve directly, cosmological simulations are crucial for understanding theirformation. Here we quantify the rates and locations of low metallicity starformation using the high-resolution TNG50 magnetohydrodynamical cosmologicalsimulation, and we examine where low metallicity stars end up at $z=0$. We findthat $20\%$ of stars with $Z_*<0.1\,\mathrm{Z_\odot}$ form after $z=2$, andthat such stars are still forming in galaxies of all masses at $z=0$ today.Moreover, most low-metallicity stars at $z=0$ reside in massive galaxies. Weanalyse the radial distribution of low metallicity star formation, and discussthe curious case of seven galaxies in TNG50 that form stars from primordial gaseven at $z=0$.

Formation and fate of low metallicity stars in IllustrisTNG50