Table 7
Comparison of our SFR estimates and the ones derived by changing one of the model descriptions outlined in Sect. 6.
| Module | All | StarForm | AGN | |||
|---|---|---|---|---|---|---|
| Δ | NMAD | Δ | NMAD | Δ | NMAD | |
| IMF (Chabrier 2003 vs. Salpeter 1955) | −0.212 | 0.314 | −0.198 | 0.292 | −0.209 | 0.309 |
| SSP (Bruzual & Charlot 2003 vs. Maraston 2005) | −0.214 | 0.462 | −0.256 | 0.384 | −0.227 | 0.389 |
| SFH (delayed with extra burst vs non parametric) | 1.018 | 2.636 | 1.664 | 2.503 | 1.303 | 2.24 |
| Z (metallicity fixed to solar vs. variable) | 0.217 | 0.598 | 0.064 | 0.146 | 0.163 | 0.374 |
| DustAtt (Calzetti et al. 2000 vs. Charlot & Fall 2000) | 0.047 | 0.171 | 0.012 | 0.096 | 0.052 | 0.198 |
| DustEm (Draine et al. 2014 vs. Dale et al. 2014) | −0.009 | 0.097 | −0.007 | 0.051 | −0.003 | 0.184 |
| AGN (Fritz et al. 2006 vs. no AGN) | −0.142 | 0.220 | −0.049 | 0.075 | −0.190 | 0.287 |
| AGN (Fritz et al. 2006 vs. Stalevski et al. 2012, 2016) | 0.008 | 0.038 | 0.002 | 0.010 | 0.044 | 0.127 |
| SEDs (grzW14 vs. grzW12) | 0.023 | 0.481 | 0.034 | 0.180 | 0.321 | 0.928 |
| SEDs (grzW14 vs. grz) | −0.540 | 1.022 | −0.302 | 0.542 | −0.298 | 0.841 |
| SFR (SED(Salpeter 1955) vs. Hα) | 0.119 | 0.567 | 0.136 | 0.413 | 0.248 | 0.871 |
Notes. The Δ, and NMAD (see Sect. 5.1 for definitions) are reported for the given change in the model considering a change in the initial mass function (IMF), single stellar population models (SSP), star formation history prescription (SFH), metallicity (Z), dust attenuation law (DustAtt), dust emission model (DustEm), and AGN models (AGN). The influence of the presence of MIR information and comparison with SFR derived based on the Hα emission line are also reported. The metrics are derived for the entire representative sample (All) and separately for star-forming galaxies (StarForm) and AGN (including both NL and BL AGNs).
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