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Aims . We aim to understand the physical mechanisms that drive star formation in a sample of mass-complete (>10 9.5 M ⊙ ) star-forming galaxies (SFGs) at 1.2 ≤ ɀ 0.7) have a mean molecular gas fraction ~2.1 times larger and mean molecular gas depletion time ~3.3 times shorter than MS galaxies. Additionally, they have more compact star-forming regions (~2.5 kpc for MS galaxies vs. ~1.4 kpc for SBs) and systematically disturbed rest-frame optical morphologies, which is consistent with their association with major-mergers. SBs and MS galaxies follow the same relation between their molecular gas mass and star formation rate surface densities with a slope of ~ 1.1–1.2, that is, the so-called Kennicutt-Schmidt relation.
Wang et al. (Mon,) studied this question.