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tokens: object. This is because we need it for the de-blending process, but it is excluded from the rest of the analysis. For the rest of the region, we had to use a different tracer. Good examples are either 24 m (e.g. Marsden et al. 2009 ; Pascale et al. 2009 ; Elbaz et al. 2010 ; Béthermin et al. 2012 ) or radio (e.g. Ivison et al. 2010 ; Magnelli et al. 2010 ; Basu et al. 2015 ; Rujopakarn et al. 2016 ; Delhaize et al. 2017 ). Even though an MIPS 24 m map was available, the beam size is still large (∼6 arcsec) and galaxies will still be blended. Instead we used the 10 cm (3 GHz) JVLA map as our tracer, as it has resolution comparable to that of our ALMA map. We identified 319 significant sources in the radio map (within the same area of the SCUBA-2 maps), and combine these with the 12 ALMA sources. These sources were then passed through XID+ to obtain fluxes for both the PACS and SPIRE maps. A specially modified version of XID+ was used to work with the SCUBA-2 maps, so we also have de-blended fluxes for both 450 and 850 m. 3.3 Association with radio sources We then went about associating each of our SCUBA-2 sources with at least one radio source (and therefore can associate with optical and NIR sources). To determine the most likely radio source we use the standard Poissonian probability of positional match similar to the method outlined in Downes et al. ( 1986 ). This value P gives us the probability of a source not being associated with the SCUBA-2 source and is given by where n is the number density of sources in the radio map, and θ is the separation between the SCUBA-2 source and the radio source. We found all radio sources within 15 arcsec of the SCUBA-2 source, and calculated the P value for all of them. For galaxies that had similar P values we picked the source that was reddest in the IRAC bands, as it has been shown that sub-mm galaxies tend to be redder at these wavelengths (e.g. Ashby et al. 2006 ; Yun et al. 2008 ; Hainline et al. 2009 ). We did not worry about the central source (source 850_1) as we use the ALMA sources from C18 , which have been shown to have association with optical and NIR sources. Using the prescriptions laid out in Ivison et al. ( 2002 ), Chapin et al. ( 2009 ), and Chen et al. ( 2016 ), we considered a reliable match to have a P ≤ 0.05 and a tentative match to have 0.05 ≤ P ≤ 0.1. Anything with a P > 0.1 is considered an untrustworthy match and removed. We found that all but two sources had either reliable or tentative matches, with 850_12 and 850_19 having sources too far to be considered significant. Even though 850_18 and 850_28 had low P values, in the optical and NIR images they were obscured by nearby stars and hence removed from the sample. Finally 850_30 was removed because there was no radio source within 15 arcsec. Applying these cuts we ended up with 37 sources that we can calculate redshifts for, and determine if they are likely to be within the cluster or not. 4 REDSHIFT DETERMINATION To