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abstract: 'We present the first cross-correlation measurement between Sloan Digital Sky Survey (SDSS) Type 1 quasars and the cosmic infrared background (CIB) measured by [*Herschel*]{}-SPIRE. The distribution of the quasars at $0.15<z<3.5$ covers the redshift range where we expect most of the CIB to originate. We detect the sub-millimetre (sub-mm) emission of the quasars, which dominates on small scales, as well as correlated emission from dusty star-forming galaxies (DSFGs) dominant on larger scales. A simple halo model is used to interpret the measured cross-correlation signal. The mean sub-mm flux densities of the DR7 quasars (median redshift $\left<z\right>=1.4$) is $11.1^{+1.6}_{-1.4}$, $7.1^{+1.6}_{-1.3}$ and $3.6^{+1.4}_{-1.0}$ mJy at 250, 350 and 500 $\micron$, respectively, while the mean sub-mm flux densities of the DR9 quasars ($\left<z\right>=2.5$) is $5.7^{+0.7}_{-0.6}$, $5.0^{+0.8}_{-0.7}$ and $1.8^{+0.5}_{-0.4}$ mJy. We find that the correlated sub-mm emission includes both the emission from satellite DSFGs in the same halo as the central quasar (the one-halo term) and the emission from DSFGs in separate halos that are correlated with the quasar-hosting halo (the two-halo term). The amplitude of the one-halo term is about 10 times smaller than the sub-mm emission of the quasars, implying the the satellite DSFGs have a lower star-formation rate than 