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In this tutorial it is explained the procedure to analyze an opticalemission-line spectrum produced by a nebula ionized by massive star formation.Particularly, it is described the methodology used to derive physicalproperties, such as electron density and temperature, and the ionic abundancesof the most representative elements whose emission lines are present in theoptical spectrum. The tutorial is focused on the direct method,based on themeasurement of the electron temperature to derive the abundances, given thatthe ionization and thermal equilibrium of the ionized gas is dominated by themetallicity. The ionization correction factors used to obtain total abundancesfrom the abundances of some of their ions are also given. Finally, somestrong-line methods to derive abundances are described. These are used when noestimation of the temperature can be derived, but that can be consistent withthe direct method if they are calibrated.

Ionized gaseous nebulae chemical abundance determination using the direct method