Fluorine in the Galaxy and the Large Magellanic Cloud

Astronomy and Astrophysics – Astronomy

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Stellar Abundances

Scientific paper

The behaviour of fluorine with metallicity has not yet been probed in any stellar population. To date fluorine abundances have only been measured in a few K and M giant stars with near-solar matallicities in our Galaxy. The origins of fluorine are still uncertain and could be due to perhaps three sources: 1) neutrino induced nucleosynthesis happening in core-collapse supernovae 2) asymptotic giant branch stars undergoing He-burning thermal pulses or 3) mass-loss from He-burning regions in Wolf-Rayet stars. In this work we present first results for fluorine abundances in a sample of red giants from the Galactic disk M4 Omega Centauri and the LMC from spectra obtained with Phoenix on Gemini South. The observed IR spectra contain HF molecular lines. If fluorine is produced by Wolf-Rayet stars its yield is predicted to be a strong positive function of metallicity. In such a case fluorine abundances derived in DLA systems could test for chemical evolution driven by Wolf-Rayet stars.

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