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tokens: fact is also illustrated in Fig. 12 , where the contour plots at 75% of the population are depicted. Figure 12 shows the mass range split over four bins for DAE diagram on the top row, for the PCA at the center, and for the RJ NUVR diagram on the bottom row. We note that the overlap is significantly lower for the DAE diagram, compared to the PCA diagram and to the RJ NUVR plane. The data-driven representations present a clear evolution over the axis in terms of mass for both star-forming and quiescent populations, while this evolution is barely observed in the classical RJ NUVR diagram. These distinct behaviors of the stellar mass distributions in the diagrams thus reveal variations of the galaxy SED properties that are again more efficiently extracted with the unsupervised learning techniques than when just taking the NUV and rest-frame colors into consideration. Given that the stellar mass of galaxies tightly correlates with their near-infrared luminosities, the mass distributions observed in Fig. 9 may suggest that the PCA and the DAE results at a given redshift are partially driven by the variations of the near-IR magnitudes that can be probed at this kind of redshift. On the other hand, the stellar mass also correlates with other physical properties such as the dust extinction and the activity of star formation, which both modify the overall shape of galaxy SEDs and necessarily also impact the DAE outputs. For instance, galaxies with enhanced recent star formation display SEDs characterized by a more important contribution of young and massive stars, which produces intense radiations of UV photons boosting the overall galaxy emission at short wavelengths. The star formation rate (SFR) of galaxies also correlates with their stellar mass, but in a non-linear relation such that the SFR per unit of mass mildly decreases in more massive sources ( Speagle et al. 2014 ). The relative level of star-forming activity in galaxies could thus also contribute to the apparent variation of the DAE and PCA distributions with the stellar mass. Fig. 12 Contour plots for different mass bins on the DAE diagram, on the PCA diagram and on the RJ – NUVR plane. The mass range is split over four bins and the contour plots are displayed at of the samples in the different mass bins. The DAE diagram is displayed on the top, PCA diagram at the center, and the RJ NUVR diagram on the bottom. The contour’s colors grow from grey to green for star-forming galaxies, and from yellow to purple for quiescent galaxies, respectively. These plots attest to the relationship with the stellar mass captured by the DAE and PCA diagrams for both star-forming and quiescent populations, while the overlap in the RJ – NUVR diagram is considerably higher. 4.3. Specific star formation rate To further explore the impact of the galaxy star-forming activity in the different diagrams, we conducted a similar analysis, taking into consideration this time the influence of the specific star