  Gas-phase abundances in HII regions of two spiral galaxies, NGC7793 and
NGC4945, have been studied to determine their radial metallicity gradients. We
used the strong-line method to derive oxygen abundances from spectra acquired
with GMOS-S, the multi-object spectrograph on the 8m- Gemini South telescope.
We found that NGC7793 has a well-defined gas-phase radial oxygen gradient of
-0.321 $\pm$ 0.112 dex R$_{\rm 25}^{-1}$ (or -0.054 $\pm$ 0.019 dex kpc$^{-1}$)
in the galactocentric range 0.17$<$R$_{\rm G}$/R$_{\rm 25}$ $<$ 0.82, not
dissimilar from gradients calculated with direct abundance methods in galaxies
of similar mass and morphology. We also determined a shallow radial oxygen
gradient in NGC4945, -0.253 $\pm$ 0.149 dex R$_{\rm 25}^{-1}$ (or -0.019 $\pm$
0.011 dex kpc$^{-1}$) for 0.04$<$R$_{\rm G}$/R$_{\rm 25}$ $<$ 0.51, where the
larger relative uncertainty derives mostly from the larger inclination of this
galaxy. NGC7793 and NGC4945 have been selected for this study because they are
similar, in mass and morphology, to M33 and the Milky Way, respectively. Since
at zeroth order we expect the radial metallicity gradients to depend on mass
and galaxy type, we compared our galaxies in the framework of radial
metallicity models best suited for M33 and the Galaxy. We found a good
agreement between M33 and NGC7793, pointing toward similar evolution for the
two galaxies. We notice instead differences between NGC4945 and the radial
metallicity gradient model that best fits the Milky Way. We found that these
differences are likely related to the presence of an AGN combined with a bar in
the central regions of NGC4945, and to its interacting environment.
