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Fig. 4


Two typical spectra of H ii regions observed in the sample with different levels of stellar contribution. The black line represents the observed spectrum, along with the best fitted stellar population performed by FIT3D (SSP model, red line). The pure emission line spectrum after subtracting the SSP model is shown as a blue line. The insets are focussed on the Hβ and Hα−NII spectral regions to highlight the quality of both the spectra and the subtraction of the underlying stellar continuum.

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