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{{short description|The distribution within a group of stars of the ratio of iron to hydrogen in a star}}
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>{{cite journal |last1=Fenner |first1=Yeshe |last2=Gibson |first2=Brad K. |title=Deriving the Metallicity Distribution Function of Galactic Systems |journal=Publications of the Astronomical Society of Australia |date=5 March 2013 |volume=20 |issue=2 |pages=189–195 |doi=10.1071/AS02047 |url=http://www.publish.csiro.au/?act=view_file&file_id=AS02047.pdf|arxiv=astro-ph/0304320 |bibcode=2003PASA...20..189F |s2cid=9965955 }}</ref><ref name=Casagrande>{{cite journal |last1=Casagrande |first1=L. |last2=Schönrich |first2=R. |last3=Asplund |first3=M. |last4=Cassisi |first4=S. |last5=Ramírez |first5=I. |last6=Meléndez |first6=J. |last7=Bensby |first7=T. |last8=Feltzing |first8=S.|author8-link= Sofia Feltzing |title=New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s) |journal=Astronomy & Astrophysics |date=26 May 2011 |volume=530 |pages=A138 |doi=10.1051/0004-6361/201016276 |url=http://www.aanda.org/articles/aa/pdf/2011/06/aa16276-10.pdf|arxiv=1103.4651 |bibcode=2011A&A...530A.138C |s2cid=56118016 }}</ref><ref name=Frinchaboy>{{cite journal|last1=Frinchaboy|first1=P. M.|last2=Rhee|first2=J.|last3=Ostheimer|first3=J. C.|last4=Majewski|first4=S. R.|last5=Patterson|first5=R. J.|last6=Johnson|first6=W. Y.|last7=Dinescu|first7=D. I.|last8=Palma|first8=C.|last9=Westfall|first9=K. B.|title=The Metallicity Distribution Function of omega Centauri|journal=Omega Centauri|date=2002|volume=265|pages=143|arxiv=astro-ph/0112169 |bibcode=2002ASPC..265..143F}}</ref><ref name=Halo-Beers-2005>{{Cite journal |arxiv=astro-ph/0508423 |last1=Beers |first1=Timothy C |title=The Metallicity Distribution Function of the Halo of the Milky Way |journal=Proceedings of the International Astronomical Union |volume=1 |pages=175–183 |last2=Christlieb |first2=Norbert |last3=Norris |first3=John E |last4=Bessell |first4=Michael S |last5=Wilhelm |first5=Ronald |author6=Carlos Allende Prieto |last7=Yanny |first7=Brian |last8=Rockosi |first8=Constance |author9=Heidi Jo Newberg |last10=Rossi |first10=Silvia |author11=Young Sun Lee |year=2005 |doi=10.1017/S1743921305005521|bibcode=2005IAUS..228..175B |s2cid=18380786 }}</ref><ref name=M31-Sarajedini-2005>{{Cite journal |arxiv=astro-ph/0506653 |last1=Sarajedini |first1=Ata |title=The Metallicity Distribution Function of Field Stars in M31's Bulge |journal=The Astronomical Journal |volume=130 |issue=4 |pages=1627–1634 |last2=Jablonka |first2=Pascale |year=2005 |doi=10.1086/433171|bibcode=2005AJ....130.1627S |s2cid=17051527 }}</ref><ref name=Shlesinger-2011>{{Cite journal |arxiv=1112.2214 |last1=Schlesinger |first1=Katharine J |title=The Metallicity Distribution Functions of SEGUE G and K dwarfs: Constraints for Disk Chemical Evolution and Formation |journal=The Astrophysical Journal |volume=761 |issue=2 |pages=160 |last2=Johnson |first2=Jennifer A |last3=Rockosi |first3=Constance M |author4=Young Sun Lee |last5=Morrison |first5=Heather L |last6=Schoenrich |first6=Ralph |author7=Carlos Allende Prieto |last8=Beers |first8=Timothy C |last9=Yanny |first9=Brian |last10=Harding |first10=Paul |last11=Schneider |first11=Donald P |last12=Chiappini |first12=Cristina |last13=da Costa |first13=Luiz N |last14=Maia |first14=Marcio A. G |last15=Minchev |first15=Ivan |last16=Rocha-Pinto |first16=Helio |last17=Santiago |first17=Basilio X |year=2011 |doi=10.1088/0004-637X/761/2/160|bibcode=2012ApJ...761..160S |s2cid=119205318 }}</ref><ref name=Yong2012>{{cite journal |title=The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction |journal=The Astrophysical Journal |first1=David |last1=Yong |first2=John E. |last2=Norris |first3=M. S. |last3=Bessell |first4=N. |last4=Christlieb |first5=M. |last5=Asplund |first6=Timothy C. |last6=Beers |first7=P. S. |last7=Barklem |first8=Anna |last8=Frebel |first9=S. G. |last9=Ryan |date=1 January 2013 |volume=762 |issue=1 |pages=27 |doi=10.1088/0004-637X/762/1/27 |arxiv = 1208.3016 |bibcode = 2013ApJ...762...27Y |s2cid=16930550 }}</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>{{cite web |url=http://www.astro.bas.bg/~petrov/holzman07_files/ay616/node5.html |title=Chemical evolution models |work=bas.bg |accessdate=3 March 2017}}</ref><ref>{{Cite journal |arxiv=1106.2168 |title=<nowiki>The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy</nowiki> |journal=The Astrophysical Journal |volume=738 |pages=51 |last1= Lai |first1=David K. |author2=Young Sun Lee |last3=Bolte |first3=Michael |last4=Lucatello |first4=Sara |last5= Beers |first5=Timothy C. |last6= Johnson |first6=Jennifer A. |last7=Sivarani |first7=Thirupathi |last8= Rockosi |first8=Constance M. |author-link8=Constance M. Rockosi |year=2011 |issue=1 |doi=10.1088/0004-637X/738/1/51 |bibcode = 2011ApJ...738...51L |s2cid=118627008 }}</ref>
==See also==
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