Mean stellar population and dust properties in the SFR_100 Myrs–M_⋆ plane of our primary sample. Panels from left to right display: mass-weighted stellar age (t_⋆, mw), stellar metallicity (Z_⋆), dust optical depth in the V band (${\widehat{\tau }}_{\mathrm{dust},2}$), and dust attenuation slope index (n). Top row: Individual data points, with typical error bars shown in the bottom-right corner of each panel. Middle row: Average trends of the physical properties across the SFR_100 Myrs–M_⋆ plane, derived using the LOESS method. Bottom row: Average upper uncertainties for each property. Each hexbin includes a minimum of five galaxies. The SFS at z = 0.60 is indicated by the solid black line, following the definition of Leja et al. (2022), while the dashed black line represents the boundary between star-forming and quiescent galaxies (sSFR = 10⁻¹¹ yr⁻¹). In the middle row, black markers indicate the median SFR_100 Myrs values in bins of M_⋆: open stars for star-forming galaxies and open circles for quiescent galaxies (see Table 2). Additionally, results from previous studies at a similar redshift range are overplotted for comparison.