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Fig. 9.


The best-fit star formation sequence for the 179 star-forming galaxies observed with MUSE. The symbols indicate the dust-corrected tracer used to infer the SFR. The solid line shows best-fit relation, as presented in Eq. (11), and the dashed lines show the 1σ intrinsic scatter. We subtract the evolution from the y-axis and scale to the average redshift of the sample; z = 0.55. After accounting for evolution, the galaxies clearly follow the star formation sequence, down to the lowest masses and SFRs. The slightly larger fraction of galaxies that scatter into the high-mass, low-SFR regime may be a result of the flattening of the relation above M* = 1010M.

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