Figures

 
Figure 1: The relationship between the [O III] luminosity and the radio luminosity for both radio-quiet and radio-loud classes of AGN drawn from the literature (Bicknell, Dopita and Tsvetanov 1997, in prep). This can be considered as the ``Hertzprung-Russell'' diagram for AGN evolution. We envision that BHs in spiral hosts remain on the radio-quiet side of the diagram, unless they are involved in a major merger, in which case rapid growth of the BH occurs (IRAS ``60m peakers''), before the AGN rapidly passes through the intermediate radio-loud IRAS galaxy phase to become a radio-loud massive BH in an elliptical host galaxy. Subsequent merges with low-mass companion galaxies cause it to be reborn as a GPS or CSS galaxy, and later, as an FR II radio galaxy. As accretion decreases, or if the AGN is fed by a cooling flow, the AGN appears as a LINER / FR I / BL Lac object.

 
Figure 2: The factor by which the nuclear feeding exceeds the Eddington value for the Black Hole, for the case = 10 and = 5 (solid), 3(long dash) and 1 (short dash). With = 10 the period of overfeeding is longer, and rises as high as 3.5.

 
Figure 3: The mass of the BH compared to its initial value as a function of time for the three cases of figure 2.

 
Figure 4: The proposed unification scheme according to aspect, accretion rate black hole mass and evolutionary status.

© Copyright Astronomical Society of Australia 1997