  We present a new analysis of the PG quasar sample based on Spitzer and
Herschel observations. (I) Assuming PAH-based star formation luminosities
(L_SF) similar to Symeonidis et al. (2016, S16), we find mean and median
intrinsic AGN spectral energy distributions (SEDs). These, in the FIR, appear
hotter and significantly less luminous than the S16 mean intrinsic AGN SED. The
differences are mostly due to our normalization of the individual SEDs, that
properly accounts for a small number of very FIR-luminous quasars. Our median,
PAH-based SED represents ~ 6% increase on the 1-243 micron luminosity of the
extended Mor & Netzer (2012, EM12) torus SED, while S16 find a significantly
larger difference. It requires large-scale dust with T ~ 20 -- 30 K which, if
optically thin and heated by the AGN, would be outside the host galaxy. (II) We
also explore the black hole and stellar mass growths, using L_SF estimates from
fitting Herschel/PACS observations after subtracting the EM12 torus
contribution. We use rough estimates of stellar mass, based on scaling
relations, to divide our sample into groups: on, below and above the star
formation main sequence (SFMS). Objects on the SFMS show a strong correlation
between star formation luminosity and AGN bolometric luminosity, with a
logarithmic slope of ~ 0.7. Finally we derive the relative duty cycles of this
and another sample of very luminous AGN at z = 2 -- 3.5. Large differences in
this quantity indicate different evolutionary pathways for these two
populations characterised by significantly different black hole masses.
