Extended Data Fig. 5: The relation between MBH and M* for local (zâ<â0.1) type 2 AGNs.
From: Evolutionary paths of active galactic nuclei and their host galaxies
BH masses are derived from broad emission lines in the near-infrared (see Methods). Their evolution to zâ=â0 is indicated by the direction and length of each arrow. Best-fit relations from ref. 5 for local early-type galaxies (black dashed line), late-type galaxies (black dotted line), and both types combined (black solid line; intrinsic scatter of 0.81 dex indicated as shaded gray region). Typical uncertainties are shown in the lower-right corner.
