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tokens: 5 and 6 arcmin from each cluster centroid generated a set of background values distributed symmetrically about the global background computed in Section 4.2 with no evidence of clusters with high MIR aperture flux measurements displaying enhanced local background values. Identification of X-ray faint, MIR bright clusters in Fig. 2 is therefore not influenced by the application of a global background correction to MIR cluster aperture fluxes. It is furthermore unlikely that the non-cluster masking procedure applied to the computation of X-ray aperture fluxes results in the exclusion of bona-fide cluster flux from the aperture measurement. As mentioned previously, XMM–LSS pipeline detections corresponding to non-C1/C2 sources were masked from the aperture measurement. An alternative masking procedure was tested, this time excluding source areas corresponding only to point sources classified as P1 (high significance, low extension), with little or no qualitative difference in the results presented above. We also compare the X-ray and MIR brightness measures of each cluster sample in terms of their luminosity using the measured redshift for each cluster and the assumed cosmological model to convert the measured aperture flux in either the X-ray or IRAC1 band, respectively, to a rest-frame [0.5–2] keV X-ray and K -band stellar luminosities. In addition to the luminosity distance to each source, the correction to luminosity requires the application of a k -correction. For the X-ray brightness, this correction is computed using the same T = 2 keV plasma model used to convert count rates to flux. In the MIR, we employ a k -correction derived from a 1 Gyr, solar metallicity burst of star formation which evolves passively from a formation redshift z f = 10.This model is taken from Willis et al. ( 2013 ) and matches the red-sequence evolution of the XMM–LSS distant cluster sample. Furthermore, as demonstrated by van der Burg et al. ( 2014 ), the stellar mass in SpARCS distant clusters is dominated by M * galaxies located on the red sequence. The evolving spectrum was realized using the galaxev 2003 stellar population synthesis code (Bruzual Charlot 2003 ). Computing theMIRluminosityof a galaxy cluster within a spatial aperture effectively involves integrating the cluster galaxy luminosity function (LF) down to a sensitivity limit which itself may be expected to be a function of redshift. In order to determine whether this is likely to be an important bias in the aperture luminosity values computed for this , we performed the following analysis: taking the 3.6 m flux limit of the optical–MIR catalogue as 3.7 μJy, we computed the corresponding K -band luminosity of a galaxy with this flux over the redshift interval 0.8 z 1.6 (the extent of the SpARCS sample). We next considered this luminosity as the limiting value as a function of redshift to which we integrated the K -band cluster galaxy LF presented by De Propris et al. ( 2007 ). The relative change in