Golden mass determined from the central M_DM/M_⋆ − M_⋆ relation assuming the reference CAMELS simulation (green line) is compared with other results from the literature. A qualitative range for the golden mass values determined from all the CAMELS simulations explored in this paper are shown as dark and light green regions (see text for more details). We also plot the results for the simulations corresponding to the lowest BH_RE and highest A_SN1 values. Then, we compare with the golden mass estimated from the same correlation for the TNG100-1 (dark green line) and TNG300-1 (dashed dark green line) simulations. From the theoretical point of view, we also show the shock heating stellar mass (M_shock) as a red line and the stream mass (M_stream) as solid cyan line (Dekel & Birnboim 2006), together with its two revised forms (dashed and dotted cyan lines) discussed in Daddi et al. (2022a). These curves for M_shock and M_stream are extracted from Daddi et al. (2022a), where more details can be found. The stream mass determined in Waterval et al. (2025) is also plotted as blue and dark blue lines (see details in the text). We show the typical mass above which SN feedback interrupts its quenching effect, using two conversions from halo to stellar mass (M_SN, yellow lines; see text for details). From the observational point of view, we plot the range of golden masses in the local Universe from different observables (Tortora et al. 2010, 2016, 2019). Then, we also plot the stellar mass value of the bending in the SHMR determined from using halo-abundance matching in Moster et al. (2010, black dashed line), Moster et al. (2013, black solid line) and Girelli et al. (2020, grey solid line), and the bending mass in the main sequence of star-forming galaxies (Lee et al. 2015; Delvecchio et al. 2021; Euclid Collaboration: Enia et al. 2025).