Trends (or lack thereof) of the measured properties with galactocentric distance. ⟨ t_⋆ ⟩_M (top), log M_⋆ (second row), SFR (third row) and A_V (bottom) of clumps and complexes are plotted against the normalized log distance log d/R_e to the center of the host galaxy. The different panels show clumps selected from Hα (left) and F275W (middle), as well as star-forming complexes (right). Black points trace the median values of physical properties in bins of log d/R_e and vertical lines indicate interquartile regions, points are plotted in the center of each bin. In the third row of panels, only objects within ±1 dex of the sequence shown in Fig. 5 are included as points, histograms show the distribution of objects below (dashed line) and within (solid line) ±1 dex of the sequence. In the bottom row we show only objects that formed a significant fraction of their stellar mass in the past 20 Myr (classified as late decliners in Sect. 3.3).