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We carry out a comparative analysis of the metallicities from the stellar,neutral-gas, and ionized-gas components in the metal-rich spiral galaxy M83. Weanalyze spectroscopic observations taken with the Hubble Space Telescope (HST),the Large Binocular Telescope (LBT) and the Very Large Telescope (VLT). Wedetect a clear depletion of the HI gas, as observed from the HI columndensities in the nuclear region of this spiral galaxy. We find column densitiesof log[$N$(HI) cm$^{-2}$] $<$ 20.0 at galactocentric distances of $<$ 0.18 kpc,in contrast to column densities of log[$N$(HI) cm$^{-2}$] $\sim$ 21.0 in thegalactic disk, a trend observed in other nearby spiral galaxies. We measure ametallicity gradient of $-$0.03 $\pm$ 0.01 dex kpc$^{-1}$ for the ionized gas,comparable to the metallicity gradient of a local benchmark of 49 nearbystar-forming galaxies of $-$0.026 $\pm$ 0.002 dex kpc$^{-1}$. Our co-spatialmetallicity comparison of the multi-phase gas and stellar populations showsexcellent agreement outside of the nucleus of the galaxy hinting at a scenariowhere the mixing of newly synthesized metals from the most massive stars in thestar clusters takes longer than their lifetimes ($\sim$10 Myr). Finally, ourwork shows that caution must be taken when studying the metallicity gradient ofthe neutral-gas component in star-forming galaxies, since this can be stronglybiased, as these environments can be dominated by molecular gas. In theseregions the typical metallicity tracers can provide inaccurate abundances asthey may trace both the neutral- and molecular-gas components.

First Co-spatial Comparison of Stellar, Neutral-, and Ionized-gas Metallicities in a metal-rich galaxy: M83