  Recoiling supermassive black holes (SMBHs) are considered one plausible
physical mechanism to explain high velocity shifts between narrow and broad
emission lines sometimes observed in quasar spectra. If the sphere of influence
of the recoiling SMBH is such that only the accretion disc is bound, the dusty
torus would be left behind, hence the SED should then present distinctive
features (i.e. a mid-infrared deficit). Here we present results from fitting
the Spectral Energy Distributions (SEDs) of 32 Type-1 AGN with high velocity
shifts between broad and narrow lines. The aim is to find peculiar properties
in the multi-wavelength SEDs of such objects by comparing their physical
parameters (torus and disc luminosity, intrinsic reddening, and size of the
12$\mu$m emitter) with those estimated from a control sample of $\sim1000$
\emph{typical} quasars selected from the Sloan Digital Sky Survey in the same
redshift range. We find that all sources, with the possible exception of
J1154+0134, analysed here present a significant amount of 12~$\mu$m emission.
This is in contrast with a scenario of a SMBH displaced from the center of the
galaxy, as expected for an undergoing recoil event.
