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We analyze the redshift evolution of the mass-metallicity relation in asample of 110 Damped Ly$\alpha$ absorbers spanning the redshift range$z=0.11-5.06$ and find that the zero-point of the correlation changessignificantly with redshift. The evolution is such that the zero-point isconstant at the early phases of galaxy growth (i.e. no evolution) but thenfeatures a sharp break at $z=2.6\pm 0.2$ with a rapid incline towards lowerredshifts such that damped absorbers of identical masses are more metal rich atlater times than earlier. The slope of this mass metallicity correlationevolution is $0.35 \pm 0.07$ dex per unit redshift.  We compare this result to similar studies of the redshift evolution ofemission selected galaxy samples and find a remarkable agreement with the slopeof the evolution of galaxies of stellar mass log$(M_{*}/M_\odot) \approx 8.5$.This allows us to form an observational tie between damped absorbers andgalaxies seen in emission.  We use results from simulations to infer the virial mass of the dark matterhalo of a typical DLA galaxy and find a ratio $(M_{vir}/M_{*}) \approx 30$.  We compare our results to those of several other studies that have reportedstrong transition-like events at redshifts around $z=2.5-2.6$ and argue thatall those observations can be understood as the consequence of a transitionfrom a situation where galaxies were fed more unprocessed infalling gas thanthey could easily consume to one where they suddenly become infall starved andturn to mainly processing, or re-processing, of previously acquired gas.

monthly notices of the royal astronomical society

Mass-metallicity relation from z=5 to the present: Evidence for a  transition in the mode of galaxy growth at z=2.6 due to the end of sustained  primordial gas infall