The ADF and the t$^2$ formalism in H II regions based on the upper mass
  limit of the IMF for the MW
  We study in depth the abundance discrepancy problem in H II regions, this
time from a different perspective than the usual one: by studying the effect of
the upper mass limit (M$_{\rm up}$) of the initial mass function (IMF) on the
O, C, and He predicted by chemical evolution models for the Milky Way. We use
abundances determined with the direct method (DM) and with the temperature
independent method (TIM). We compare the predicted abundances at the present
time with observations of Orion, M17, and M8 to determine the M$_{\rm up}$
value of the galactic IMF. From the DM abundances, the models predict an
M$_{\rm up}$ = 25-45 M$_{\odot}$, while from the TIM, CEMs derive an M$_{\rm
up}$ = 70-110 M$_{\odot}$. Spiral galaxies with the stellar mass and star
formation rate of the MW are predicted to have an M$_{\rm up} \sim100$
M$_{\odot}$. These results support that abundances derived from the TIM are
better than those derived from the DM.
