A fundamental relation between mass, SFR and metallicity in local and
  high redshift galaxies
  We show that the mass-metallicity relation observed in the local universe is
due to a more general relation between stellar mass M*, gas-phase metallicity
and SFR. Local galaxies define a tight surface in this 3D space, the
Fundamental Metallicity Relation (FMR), with a small residual dispersion of
~0.05 dex in metallicity, i.e, ~12%. At low stellar mass, metallicity decreases
sharply with increasing SFR, while at high stellar mass, metallicity does not
depend on SFR. High redshift galaxies, up to z~2.5 are found to follow the same
FMR defined by local SDSS galaxies, with no indication of evolution. The
evolution of the mass-metallicity relation observed up to z=2.5 is due to the
fact that galaxies with progressively higher SFRs, and therefore lower
metallicities, are selected at increasing redshifts, sampling different parts
of the same FMR. By introducing the new quantity mu_alpha=log(M*)-alpha
log(SFR), with alpha=0.32, we define a projection of the FMR that minimizes the
metallicity scatter of local galaxies. The same quantity also cancels out any
redshift evolution up to z~2.5, i.e, all galaxies have the same range of values
of mu_0.32. At z>2.5, evolution of about 0.6 dex off the FMR is observed, with
high-redshift galaxies showing lower metallicities. The existence of the FMR
can be explained by the interplay of infall of pristine gas and outflow of
enriched material. The former effect is responsible for the dependence of
metallicity with SFR and is the dominant effect at high-redshift, while the
latter introduces the dependence on stellar mass and dominates at low redshift.
The combination of these two effects, together with the Schmidt-Kennicutt law,
explains the shape of the FMR and the role of mu_0.32. The small metallicity
scatter around the FMR supports the smooth infall scenario of gas accretion in
the local universe.
