Scaling relations of clumps across redshifts. Top panels of each row: the CMF computed considering all (blue histogram) or only young (t_age < 50 Myr, green histogram) clumps for the redshifts considered in this study. As a reference, the black dashed line indicates the $\frac{\mathrm{d}N}{\mathrm{d}{M}_{\star }}\propto M_{\star }^{-2}$ relation, corresponding to a scale free spectrum of structure formation. The dashed orange line shows, instead, the fit to the high mass end of the CMF (log M_⋆ [M_⊙] > 3.25), with the resulting slope indicated in the top right corner of each panel. Central panels of each row: Size-mass relation as a function of redshift (blue points with error bars). In each panel, the orange dashed line corresponds to a linear fit to the data points. The grey vertical lines and bands represent the region of space where t_diss ≤ 13 Gyr, with t_diss as in Equation (12). Each line corresponds to a different assumption on R_G in Equation (12), specifically, from left to right, R_G = 18 kpc, 12 kpc, 6 kpc, and 3 kpc, while V_G = 220 km s⁻¹ to mimic the tidal field the clumps would experience if orbiting around a Milky Way like galaxy (see Section 5.5 for detail). Bottom panels of each row: relation between the clumps stellar mass and Sérsic index. In the central and bottom panels, the red solid curve connects the median R_e and n for each log M_⋆ bin. Note that the panels at z = 6.14 cover a different mass range than the others to highlight the presence of a massive clump with M_⋆ ≃ 2 × 10⁶ M_⊙.