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The '''Metallicity distribution function''' is an important concept in [[stellar evolution|stellar]] and [[galactic evolution]].
It is a curve of what proportion of stars have a particular [[metallicity]] ([Fe/H], the relative abundance of iron and hydrogen) of a population of stars such as in a cluster or galaxy.
<ref name=Fenner2003>[http://www.publish.csiro.au/?act=view_file&file_id=AS02047.pdf Deriving the Metallicity distribution function of galactic systems ] </ref><ref name=Casagrande>[http://www.aanda.org/articles/aa/pdf/2011/06/aa16276-10.pdf The Metallicity Distribution Function in the disc of the Milky Way and near the Sun] </ref><ref name=Frenchaboy>[http://cdsweb.cern.ch/record/529715/files/0112169.pdf The Metallicity Distribution Function of ω Centauri] </ref><ref name=Halo-Beers-2005>[http://arxiv.org/abs/astro-ph/0508423 The Metallicity Distribution Function of the Halo of the Milky Way] </ref><ref name=M31-Sarajedini-2005>[http://arxiv.org/abs/astro-ph/0506653 The Metallicity Distribution Function of Field Stars in M31's Bulge] </ref><ref name=Shlesinger-2011>[http://arxiv.org/abs/1112.2214 The Metallicity Distribution Functions of SEGUE G and K dwarfs: Constraints for Disk Chemical Evolution and Formation] </ref><ref name=Yong2012>[http://arxiv.org/abs/1208.3016 The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction]</ref> MDFs are used to test different theories of galactic evolution. Much of the iron in a star will have come from earlier type Ia [[supernova]]e. Other [alpha] metals can be produced in core collapse supernovae.<ref>[http://www.astro.bas.bg/~petrov/holzman07_files/ay616/node5.html Chemical evolution models]</ref><ref>{{cite web |url=http://arxiv.org/abs/1106.2168 |title=<nowiki>The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy</nowiki>}}</ref>
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