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tokens: etal. 2006 ; Hao etal. 2014 ), so one might expect that their far-IR SEDs are also unchanged. On the basis of the assumption that the intrinsic AGN emission as a function of wavelength is broadly independent of AGN luminosity [for L , 5100 or L X(210keV) 10 43.5 ergs 1 AGN] and redshift (at least up to z 3.5), my results indicate that, on average, the far-IR/submm emission in the most luminous QSOs at the tail of the 2 z 4 optical luminosity function (Richards etal. 2006 ) is primarily produced by the AGN. This implies that for such systems, the emission in the Herschel bands and longer wavelengths such as those probed by SCUBA-2 at 850m would be AGN dominated; thus, wide-area Herschel and SCUBA-2 surveys will contain a population of QSOs which are primarily powered by AGN. Moreover, the SFRs of such systems cannot be determined with X-ray to submm broad-band photometry, and other means such as IR spectral lines will need to be used. Note that this does not mean that the host galaxies of luminous QSOs do not have star formation, perhaps even a considerable amount: I calculate a 3 upper limit on the SFR of 3165 and 643M yr 1 for the two QSO samples studied here. It simply means that the contribution from star formation is not detected in the broad-band SED as it is energetically less prominent than the AGN power at all wavelengths. This conclusion is in disagreement with the work of N16 . N16 use an AGN torus template to decompose their QSO SEDs into an AGN torus component and a star-forming component. The torus template used by N16 has a steeper far-IR slope than the S16 AGN SED, falling by about 0.5dex between 50 and 70m, compared to a 0.1dex change in the S16 AGN SED. This implies that a smaller fraction of the far-IR emission is attributed to the AGN in the work of N16 , and indeed, they find that star formation is a significant contributor to emission in the Herschel bands. In S16 , however, we argued that using torus templates in SED decomposition can significantly underestimate the AGN power in the far-IR, as they often lack an extended dust component, which would, in turn, boost the contribution required from star formation. Other works which use SED decomposition to separate the AGN and star formation contributions also find that QSOs have IR luminosities systematically larger than the IR luminosity produced by a torus component (e.g. Leipski etal. 2014 ; Drouart etal. 2016 ; Gruppioni etal. 2016 ; Podigachoski etal. 2016 ). Although traditionally this has been assigned to star formation, here I argue that a significant fraction, and in some cases all, of this excess IR luminosity can be attributed to AGN-heated dust at kpc scales. Using a bolometric correction factor f = 4, where L AGN, bol f L , 5100 , and an efficiency of = 0.1 to convert AGN luminosity into black hole accretion rate (BHAR) as in N16 , I calculate a 3 upper limit on the SFR/BHAR ratio of 23 for the N16 sample and 36 for the T15 sample. However, note that higher