Work overview. From left to right and top to bottom: Labeled panels show: a) S-PLUS footprint scan over the southern hemisphere, where each light blue square represents a single S-PLUS observation (FoV of 1.4 × 1.4 deg²). b) Zoom-in on the S-PLUS field where NGC 253 is located, called field −s20s09, where an inset provides a closer view into the nuclear regions of this galaxy. Within the latter inset, there is another inset zooming in toward NGC 253’s CMZ, which is shown in the next panel. c) Here, we indicate the Hα (MUSE) emission as red contours and shaded areas, showing the strong stellar outflow observed at optical wavelengths. Complementing the latter, in the same panel, we show mainly in blue and white the integrated intensity of the CN 1–0 line at ∼113.4 GHz taken from ALCHEMI observations at 1$\stackrel{″}{.}$6 angular resolution. The leftmost bottom symbol of the beam in the same figure indicates this. The CN emission also presents features of molecular outflows, the most notorious one presumably coming from GMC 3, which is labeled (along with the other nine studied in this work) as the white framed black numbers. The GMC’s 3″ apertures are indicated by black circles and are connected to the numbers by black arrows. d) SED of GMC 5 from GalaPy (see our Fig. 3 for more details), the one with the highest signal-to-noise ratio (S/N) of the sample. Additionally, two zoomed-in insets are provided in the middle panels: Optical spectrum (obtained with MUSE) is shown in the middle-left panel e) Sub-millimeter spectrum (from ALCHEMI) is presented in the middle-right panel (f). The magenta dots on top of both spectra in panel f correspond to the photometric observations listed in Table 2. Key emission lines are labeled in both spectra for reference. Finally, the bottom panel (g), and its legend in the rightmost position of the figure, summarizes the transmission curves of all the observations used in this work to perform the SED fits at 3″ apertures. We also include in panel g the Herschel PACS transmission curves described in Sect. 5.1.