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Galaxies are expected to accrete pristine gas from their surroundings tosustain their star formation over cosmic timescales. Its lower abundanceaffects the metallicity of the ISM in which stars are born, leaving chemicalimprints in the stellar populations. We measure the amount of pristine gas thatgalaxies accrete during their lifetime, using information on the ages andabundances of their stellar populations and a chemical evolution model. We alsoaim to determine the efficiency of star formation over time. We derived starformation histories and metallicity histories for a sample of 8523 galaxiesfrom the MaNGA survey. We use the former to predict the evolution of themetallicity in a closed-box scenario, and estimate for each epoch the gasaccretion rate required to match these predictions with the measured stellarmetallicity. Using only chemical parameters, we find that the history of gasaccretion depends on the mass of galaxies. More massive galaxies accrete moregas and at higher redshifts than less massive galaxies, which accrete their gasover longer periods. We also find that galaxies with a higher star formationrate at z = 0 have a more persistent accretion history for a given mass. Thestar formation efficiency shows similar correlations: early-type galaxies andhigher-mass galaxies had a higher efficiency in the past, and it declined suchthat they are less efficient in the present. Our analysis of individualgalaxies shows that compactness affects the peak star formation efficiency thatgalaxies reach, and that the slope of the efficiency history of galaxies withcurrent star formation is flat. Our results support the hypothesis that asteady and substantial supply of pristine gas is required for persistent starformation in galaxies. Once they lose access to this gas supply, star formationcomes to a halt.

Measuring the physical imprints of gas flows in galaxies I: Accretion rate histories