Chempy: A flexible chemical evolution model for abundance fitting - Do the Sun’s abundances alone constrain chemical evolution models?

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Table 3

Observations, , used to constrain the Chempy parameters.


Abbreviation	Nomenclature	Description and source

Stellar abundances


{ 1 } : [ X / H ] _{⊙ ,birth}	Sun	Protosolar abundances from Asplund et al. (2009)
{ 2 } : [ X / H ] _{B − stars}	B-stars	Nearby B-stars by Nieva & Przybilla (2012) as ISM proxy
{ 3 } : [ X / Fe ] _Arc	Arcturus	Abundances and age as derived by Ramírez & Allende Prieto (2011)

Additional constraints^a (“+”)


{ 4 } :CC / Ia	SN-ratio	CC-SN to SN Ia ratio in Sbc/d galaxies at present day (Mannucci et al. 2005)
{ 5 } :Z_Smith	Corona metallicity	Metallicity of Smith cloud measured by Fox et al. (2016)

Notes.

^(a)

We combine each stellar abundance with the SN-ratio and corona metallicity in an observational set, for example, for the Sun: {1, 4, 5} and call it “Sun+” indicating the additional constraints (which we add in order to reproduce Milky Way-like global constraints in each zone).

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