Stellar mass–SFR relation for clumps and complexes in our sample. Panels from top to bottom show the relations for Hα clumps, F275W clumps and star-forming complexes, respectively. Points are colored according to ⟨ t_⋆ ⟩_M, truncating at 10 Myr and 150 Myr, clumps containing only stars younger than 10 Myr form a relation by definition and are shown as white circles. The gray band indicates a ±1 dex range around a linear fit to the Hα relation, the dashed line shows a fit to the relation for star-forming galaxies in the Sloan Digital Sky Survey from Renzini & Peng (2015). For F275W clumps and star-forming complexes we set the lower limit of the y-axis to the 1% percentile of the SFR distribution.