the Universe. In the current paradigm of galaxy formation and evolution, quasars represent a key phase in the evolutionary history of massive galaxies. Essentially all spheroidal systems are believed to harbour massive black holes. The masses of the central SMBHs are shown to correlate with many properties of their host galaxies, e.g., the stellar velocity dispersion of the bulge, the bulge mass and the bulge luminosity (e.g., Kormendy & Richstone 1995; Magorrian et al. 1998; Ferrarese & Merritt 2000; Gebhardt et al. 2000; Tremaine et al. 2002; Kormendy et al. 2011). Present-day SMBHs are thought to have gained most of their mass via accretion during an active nuclear phase, e.g. the quasar phase. The implication is that black hole growth and star-formation activity are inextricably linked, at least for galaxies which experience ‘wet’ major mergers and a quasar-like period of rapid black hole growth (see Kormendy & Ho 2013 for a review). A probable scenario is that the galaxy initially forms in a gas-rich rotationally supported system. As the host dark matter halo grows, some mechanisms, such as major merger or disk/bar instability trigger a period of rapid, dust obscured star-formation activity (starburst) which produces a stellar bulge. At the 