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Kiloparsec-scale outflows are prevalent among luminous AGN: outflows and feedback in the context of the overall AGN population

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Figure

Figure 1. Left: the FWHM of the broadest, luminous (contributes at leastoverall population ofMullaney et al.30 per cent of the total flux; FWHM[B]) [O III] emission-line componentversus total [O III] luminosity for our IFU targets (red stars) compared to th
Table 2. Target properties.
Table 3. Infrared photometric data.
Figure 3. The infrared SEDs for each target in our sample. The flux densities used in the fitting procedure are shown as blue filled triangles (with an empty symbol
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