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We present a reassessment of the radial abundance gradients of C, N, O, Ne,S, Cl and Ar in the Milky Way using deep spectra of 33 H II regions gatheredfrom the literature, covering Galactocentric distances from 6 to 17 kpc. Thedistances of the objects have been revised using Gaia parallaxes. Werecalculate the physical conditions and ionic abundances in an homogeneous wayusing updated atomic data. All the objects have direct determination of theelectron temperature, permitting to derive their precise ionic abundances. Weanalyze and compare different ICF schemes for each element in order to obtainthe most confident total abundances. Due to the revised distances, our resultsdo not support previous claims about a possible flattening of the O/H gradientin the inner Galactic disk. We find that the Galactic N/O gradient is ratherflat, in contrast to what has been found in other spiral galaxies. The slope ofthe gradients of some elements is sensitive to the ICF scheme used, especiallyin the case of Ne. The dispersion around the fit for the gradients of C, N, O,S, Cl and Ar is of the order of the typical uncertainties in the determinationof the abundances, implying the absence of significant inhomogeneities in thechemical composition of the ionized gas phase of the ISM. We find flatgradients of log(S/O) and log(Cl/O) and very shallow or flat ones for log(Ne/O)and log(Ar/O), consistent with a lockstep evolution of Ne, S, Cl and Ar withrespect to O.

The Galactic radial abundance gradients of C, N, O, Ne, S, Cl and Ar from deep spectra of H II regions