Abstract
We derive a constraint on direct black hole formation from the evolution of [O/Fe] as function of time, during the early evolution of the Galaxy in the solar neighbourhood. Since oxygen is dominantly produced by massive stars, the evolution of [O/Fe] is an indirect observable signature of the death of massive stars. We use a detailed Galactic code that computes as function of time the chemical composition of the interstellar gas, out of which successive generations of stars are formed. From our simulations we conclude, that to fit simultaneously the observed [O/Fe] evolution and other observational constraints: (i) all massive stars (single or binary) with M > 40 M⊙ should form massive black holes with the ejection of at least 7 M⊙ of oxygen and little carbon and iron; and (ii) mass loss by stellar wind during the Luminous Blue Variable phase and/or helium burning phase is likely to be metallicity dependent.
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