Evolution of the chemical enrichment and the Mass-Metallicity relation
  in CALIFA galaxies
  We use fossil record techniques on the CALIFA sample to study how galaxies in
the local universe have evolved in terms of their chemical content. We show how
the metallicity and the mass-metallicity relation (MZR) evolve through time for
the galaxies in our sample and how this evolution varies when we divide them
based on their mass, morphology and star-forming status. We also check the
impact of measuring the metallicity at the centre or the outskirts. We find the
expected results that the most massive galaxies got enriched faster, with the
MZR getting steeper at higher redshifts. However, once we separate the galaxies
into morphology bins this behaviour is not as clear, which suggests that
morphology is a primary factor to determine how fast a galaxy gets enriched,
with mass determining the amount of enrichment. We also find that star-forming
galaxies appear to be converging in their chemical evolution, that is, the
metallicity of star-forming galaxies of different mass is very similar at
recent times compared to several Gyr ago.
