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Fig. 7.

image

Star formation ratio for each emission-line component calculated from the extinction corrected Hαλ6565 luminosity. On the x-axis (resp. y-axis), we display the SFR inferred from the strong [OIII] (weak [OIII]) component. We display the morphology (see Sect. 2.2) with different markers and indicate the BPT classification of the stronger [OIII] line as colour-coded in Fig. 1. We highlight galaxies showing off-centred weak [OIII] lines with empty markers. The dashed line corresponds to equal SFR in the two components.

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