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Differential enrichment between $\alpha$- and Fe-peak elements is known to bestrongly connected with the shape of the star formation history (SFH), the starformation efficiency (SFE), the inflow and outflow of material, and even theshape of the Initial Mass Function (IMF). However, beyond the Local Groupdetailed explorations are mostly limited to early-type galaxies due to the lackof a good proxy for [$\alpha$/Fe] in late-type ones, limiting our understandingof the chemical enrichment process. We intent to extend the explorations of[$\alpha$/Fe] to late-type galaxies, in order to understand the details of thedifferential enrichment process. We compare the gas phase oxygen abundance withthe luminosity weighted stellar metallicity in an extensive catalog of$\sim$25,000 H ii regions extracted from the Calar Alto Legacy Integral FieldArea (CALIFA) survey, an exploration using integral field spectroscopy of$\sim$900 galaxies, covering a wide range of masses and morphologies. This waywe define [O/Fe] as the ratio between both parameters, proposing it as anindirect proxy of the [$\alpha$/Fe] ratio. Results. We illustrate how the[O/Fe] parameter describes the chemical enrichment process in spiral galaxies,finding that: (i) it follows the decreasing pattern with [Fe/H] reported forthe [$\alpha$/Fe] ratio and (ii) its absolute scale depends of the stellar massand the morphology. We reproduce both patterns using two different chemicalevolution models (ChEM), considering that galaxies with different stellar massand morphology present (i) different SFHs, SFEs and different inflow/outflowrates, or (ii) a different maximum stellar mass cut for the IMF. We willexplore the differential chemical enrichment using this new proxy galaxy bygalaxy and region by region in further studies.

[$\alpha$/Fe] traced by H ii regions from the CALIFA survey: The connection between morphology and chemical abundance patterns