CO Emission, Molecular Gas, and Metallicity in Main-Sequence Star-Forming Galaxies at
arXiv:2204.06937 · doi:10.3847/1538-4357/aca46f
Abstract
We present observations of CO(3-2) in 13 main-sequence star-forming galaxies at that span a wide range in metallicity (O/H) based on rest-optical spectroscopy. We find that CO(3-2)/SFR decreases with decreasing metallicity, implying that the CO luminosity per unit gas mass is lower in low-metallicity galaxies at . We constrain the CO-to-H conversion factor () and find that inversely correlates with metallicity at . We derive molecular gas masses () and characterize the relations among , SFR, , and metallicity. At , increases and molecular gas fraction (/) decrease with increasing , with a significant secondary dependence on SFR. Galaxies at lie on a near-linear molecular KS law that is well-described by a constant depletion time of 700 Myr. We find that the scatter about the mean SFR-, O/H-, and - relations is correlated such that, at fixed , galaxies with larger have higher SFR and lower O/H. We thus confirm the existence of a fundamental metallicity relation at where O/H is inversely correlated with both SFR and at fixed . These results suggest that the scatter of the star-forming main sequence, mass-metallicity relation, and - relation are primarily driven by stochastic variations in gas inflow rates. We place constraints on the mass loading of galactic outflows and perform a metal budget analysis, finding that massive star-forming galaxies retain only 30% of metals produced, implying that a large mass of metals resides in the circumgalactic medium.
arXiv comment35 pages, 17 figures, submitted to ApJ
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