Scaling relations and baryonic cycling in local star-forming galaxies

Abstract

Gas accretion and stellar feedback processes link metal content, star formation, and gas and stellar mass (and the potential depth) in star-forming galaxies. Constraining this hypersurface has been challenging because of the need for measurements of H I and H2 gas masses spanning a broad parameter space. A recent step forward has been achieved through the Metallicity And Gas for Mass Assembly sample of local star-forming galaxies, which consists of homogeneously determined parameters and a significant quantity of dwarf galaxies, with stellar masses as low as ∼105 − 106 M⊙. Here, in the third paper of a series, we adopt a standard galactic chemical evolution model, with which we can quantify stellar-driven outflows. In particular, we constrain the difference between the mass-loading in accretion and outflows and the wind metal-loading factor. The resulting model reproduces very well the local mass–metallicity relation, and the observed trends of metallicity with gas fraction. Although the difference in mass loading between accreted and expelled gas is extremely difficult to constrain, we find indications that, on average, the amount of gas acquired through accretion is roughly the same as the gas lost through bulk stellar outflows, a condition roughly corresponding to a “gas equilibrium” scenario. In agreement with previous work, the wind metal-loading factor shows a steep increase toward lower mass and circular velocity, indicating that low-mass galaxies are more efficient at expelling metals, thus shaping the mass–metallicity relation. Effective yields are found to increase with mass up to an inflection mass threshold, with a mild decline at larger masses and circular velocities. A comparison of our results for metal loading in outflows with the expectations for their mass loading favors momentum-driven winds at low masses, rather than energy-driven ones.