Star formation rate vs. stellar mass distribution in three redshift ranges, i.e., 0.1 < z < 0.5, 0.5 < z < 1.5, and 1.5 < z < 2.5 (lower panels). Filled green and magenta circles correspond to rest-MIR detection with S/N > 75 and 10 < S/N < 75, respectively. Circles outlined by black edges are detected in the FIR by Herschel (i.e., with S/N_FIR > 5, where S/N_FIR is the signal-to-noise ratios added in quadrature from 100 to 500 μm; Le Bail et al., in prep.). Black dots show galaxies within the four CEERS red MIRI fields but which remained undetected in a MIRI bandpass that is dominated by dust emission (i.e., S/N < 10 or ). Shaded regions correspond to the distribution of all sources in the EGS, plotted using a kernel density estimator. The solid and dotted black lines show the MS of SFGs and its dispersion as inferred by Schreiber et al. (2015). Upper panels: fraction of SFGs (i.e., ΔMS > −0.5) as a function of stellar mass which are within the four CEERS red MIRI fields and are in our sample (i.e., that have at least one S/N > 10 MIRI detection dominated by dust emission). Our sample is 80% mass-complete down to M_* ∼ 10^9.5, 10^9.5, and 10¹⁰ M_⊙ at z ∼ 0.3, 1.0, and 2.0, respectively. A typical 1σ error bar for individual objects is shown in the right panel.