We present a new analysis of the PG quasar sample based on \it Spitzer and \it Herschel observations .
( \ @ slowromancap i @ ) Assuming PAH-based star formation luminosities ( L _ { SF } ) similar to \citet [ ] [ S16 ] Symeonidis2016 , 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 \sim 6 % increase on the 1 - 243 \mu m luminosity of the extended \citet [ ] [ EM12 ] Mor2012 torus SED , while S16 find a significantly larger difference .
It requires large-scale dust with T \sim 20 - 30 K which , if optically thin and heated by the AGN , would be outside the host galaxy .
( \ @ slowromancap ii @ ) We also explore the black hole and stellar mass growths , using L _ { SF } estimates from fitting \it 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 \sim 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 .