Distribution in the stellar-mass–SFR plane for our combined JWST sample. This includes both JADES galaxies presented in this work and the literature sample compiled from Nakajima et al. (2023; CEERS), Curti et al. (2023; EROs), and Bunker et al. (2023b; GN-z11), respectively. The top and right-hand inset panels show the histograms of the distribution in both parameters. The SFR for JADES galaxies is derived from BEAGLE fitting to both PRISM spectra and NIRCAM photometry (where available, and to PRISM spectra only otherwise). For CEERS galaxies, the SFRs are compiled from Nakajima et al. (2023) as inferred from the Hβ luminosity and the Kennicutt & Evans (2012) calibration, but have been here scaled down by 0.23 dex to account for the mean offset between the Hα(Hβ)-based and BEAGLE-based SFRs measured for the JADES sample (we refer to Sect. 3.2 for more details). For both ERO galaxies and GN-z11 the M_⋆ and SFR have been derived via BEAGLE fitting, consistently with what done for JADES sources. The parametrisation of the main sequence of star-formation (SFMS) at z ∼ 0 and z ∼ 6 from Popesso et al. (2023; and their extrapolation at low stellar mass, dashed line) is also shown for reference.