M_• weighted 5 GHz radio luminosity versus the soft X-ray luminosity in units of the Eddington luminosity (from the fundamental plane equation in Merloni et al. 2003). Symbol shapes as in Fig. 5. For clarity, our data are presented as open black squares. In addition, we show the data of Merloni et al. (2003, gray asterisks) and the low-luminosity AGN of Yuan et al. (2009, violet, downpointing triangles). The dashed violet line represents the fit of Yuan et al. (2009) adopted to soft X-rays. The thin gray line shows the fundamental plane of Merloni et al. (2003) adopted for the soft X-rays. The thin black dotted (dot-dashed) lines indicate constant R_X =  −1.5 (R_X =  −4.5) for typical log M_• [M_⊙]  = 6 and 10 (upper and lower line), respectively. These lines have a slope of unity. Furthermore, we present data from Hardcastle et al. (2009, stars), for which the fraction of accretion related X-ray emission could be determined. The brown-colored full stars correspond to the full X-ray and the brown open stars to the accretion-related X-ray luminosities. Upper panel: presented are RL objects, R_X >  − 2.5, according to Panessa et al. (2007). The thick, dashed light-gray line represents the fit of Li et al. (2008) to their RL BLAGN. Lower panel: presented are RQ objects, R_X ≤  − 2.5, according to Panessa et al. (2007). The thick, dashed light-gray line represents the fit of Li et al. (2008) to their RQ BLAGN. See text for details.