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tokens: model when adding the centimeter data emission with = 2.60 and with parameters of m ⋆ = 16 M ⊙ , a core of mass M c = 480 M ⊙ , and a Σ cl = 0.1 g cm −2 clump. The source detected at the Inner scale (or source 8a in Beltrán et al. 2016 ) is slightly extended at 6 cm, and it is blended with other components; however, it is a point source at 1.3 cm and 0.7 cm. Thus, it is possible that we are missing part of the flux at 6 cm, and this may explain why the models seem to overestimate the expected free–free emission at 6 cm. Our resulting protostellar mass of 16 M ⊙ is consistent with the value of of 18 M ⊙ estimated by Sánchez-Monge et al. ( 2013 ) when fitting the velocity field of the core with a rotating Keplerian disk, although they argue that this value corresponds to the total mass of a binary system in core B. Our results disfavor the models with protostellar mass and with relatively low core masses and high Σ cl clumps, because the expected free–free emission for these models is many orders of magnitude lower than the observed one. G45.47+00.05: The observed centimeter continuum emission from G45.47+00.05S (which is the dominant source in the region) is significantly higher (by a few orders of magnitude) than the predicted free–free emission from any of our IR-derived ZT models. This is despite the fact that the best two models from the ZT results already predict a rather high-mass protostar in the range of 30–50 M ⊙ embedded in a massive core, a relatively high Σ clump, and low accretion rates in the range of ∼10 −5 M ⊙ yr −1 . Among the eight sources presented in this study, this is the only case where none of the free–free models can describe the centimeter emission observed in the source. This region is also the most luminous and likely the most evolved one in this sample, which leads us to think that the radio emission from this source may be boosted by the process of photoevaporation. Photoevaporation is not yet accounted for in the TTZ model, which only considered photoionization of the magnetocentrifugally driven wind. However, as the protostar increases its mass above ∼20 M ⊙ , the ionizing radiation becomes dramatically stronger, creating a photoevaporation flow from the disk and infall envelope that is exposed by the outflow cavity wall, i.e., a wind driven by ionized gas-pressure. By enhancing the mass of ionized gas, the centimeter continuum emission is expected to be much higher than that predicted by the TTZ model without such a photoevaporation flow. IRAS 20126+4104: Including the centimeter continuum fluxes to better sample the SED, we can see in Figure 3 that the best five models seem to be overestimating the expected free–free emission. Therefore, after exploring other resulting models from the DLT17 study and the ZT models, we found a matching model with = 3.38 and = 5.42, which yields protostellar parameters of , core mass M c = 240 M ⊙ , and Σ cl = 0.1 g cm −2 . This protostellar mass is consistent with the value of