Star formation rate (SFR) of the inner regions of NGC 253’s CMZ. In the x-axis, the SFR is obtained from the H40α RRL (see Subsect. 4.3.2). In the y-axis, the SFR was obtained from the Ka EVLA band, applying the best-fitting relation from our linear regression, presented in Eq. (6). The resulting fit considering all data points (all) and per GMC (color-coded) are labeled along with the Pearson correlation coefficient, ⟨R⟩. All points include 10% uncertainties, with regression handling errors in both axes via Markov Chain Monte Carlo, as described in our Subsect. 4.2.3.