Comparison between the SFR obtained from the optical-NIR bands with those from FIR. SFR^sed are derived through the modeling of the stellar emission in the UV-to-NIR. The color code indicates the number of photometric detections for each source in the FIR band. A low number of FIR detections may influence the goodness of the FIR SED-fitting, hence the SFR^{8 − 1000 μm}, but we did not find any trend between the SFR^{8 − 1000 μm}–SFR^sed offset and the number of IR photometric detections. The blue line is a 1:1 line; the red line is the best-fit line with a slope of m = 0.92 and c = 0.24, in the log(SFR^{8 − 1000 μm}/M_⊙ yr⁻¹)=c + m log(SFR^sed/M_⊙ yr⁻¹) notation.