QSOFEED: Relationship between star formation and active galactic nuclei feedback

Open Access

Fig. 10.

Difference in the velocity offset of the [OIII] emission line and that of the host galaxy (left). The right panel shows the deconvolved W80_int values against |ΔV_diff|, where $W 80_{int} = \sqrt{W 80^{2} - W 80_{SL}^{2}}$ $W80_{\mathrm{int}}=\sqrt{W80^2 - W80_{\mathrm{SL}}^2}$ and |ΔV_diff|=ΔV_[OIII] − ΔV_SL. Grey symbols indicate objects in which no outflows were detected according to our criterium.

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