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The abundance ratios of manganese to iron in late-type stars across a widemetallicity range place tight constraints on the astrophysical production sitesof Fe-group elements. In this work, we investigate the chemical evolution of Mnin the Milky Way galaxy using high-resolution spectroscopic observations ofstars in the Galactic disc and halo stars, as well as a sample of globularclusters. Our analysis shows that local thermodynamic equilibrium (LTE) leadsto a strong imbalance in the ionisation equilibrium of Mn I and Mn II lines. MnI produces systematically (up to 0.6 dex) lower abundances compared to the MnII lines. Non-local thermodynamic equilibrium (NLTE) radiative transfersatisfies the ionisation equilibrium across the entire metallicity range, -3 <[Fe/H] < -1, leading to consistent abundances from both ionisation stages ofthe element. We compare the NLTE abundances with Galactic Chemical Evolutionmodels computed using different sources of type Ia and type II supernova (SN Iaand SN II) yields. We find that a good fit to our observations can be obtainedby assuming that a significant (~ 75%) fraction of SNe Ia stem from asub-Chandrasekhar (sub-Ch) channel. While this fraction is larger than thatfound in earlier studies (~ 50%), we note that we still require ~ 25% near-ChSNe Ia to obtain solar [Mn/Fe] at [Fe/H] = 0. Our new data also suggest higherSN II Mn yields at low metallicity than typically assumed in the literature.

astronomy and astrophysics

Observational constraints on the origin of the elements. III. Evidence  for the dominant role of sub-Chandrasekhar SN Ia in the chemical evolution of  Mn and Fe in the Galaxy