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Fig. 9.


Correlation between the Na I D resonant line, [OIII]λ5007 and Hα emission-line profiles (left, central, and right panels, respectively) and the galaxy stellar disc inclination (face-on and edge-on systems with inclination i = [0, 50] and i =  ]50, 90] in green and magenta, respectively). The spectra are extracted from the pure SF galaxies (top panels) and for the AGN subsample (bottom panels). The black and blue dashed lines show the decomposition between the narrow systemic and the broad blue-shifted components needed to best fit the data. In the sodium panels, the cyan dashed lines illustrate the emission line component consistently with the P Cygni predictions shown in the cool gas wind models of Prochaska et al. (2011) and Scarlata & Panagia (2015). The Na I D line shift clearly correlates with the galaxy inclination in both SF and AGN samples. The [OIII] and Hα emission lines are independent from the galaxy morphology, but show a strong shape variation between the SF and AGN subsamples.

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