deepest in the field. OM2008 and BI2006 have rms noises of 2.7 and 6.0 $\muup$Jy/beam respectively and all the 10C sources in these fields are detected at 1.4 GHz. The majority of the @2012rsri.confE..22G WSRT map has an rms noise of $< 15~\muup$Jy/beam and parts have an rms noise of 11 $\muup$Jy/beam. This means that it should be possible to detect the faintest sources in the complete 10C sample (with $S_{15.7 \rm{GHz}} \geqslant 0.5~$mJy) in the WSRT map provided they have spectral indices $\alpha^{15.7}_{1.4} > -1$ (where $S \propto \nu ^{-\alpha}$), assuming a 3$\sigma$ WSRT detection. Sources with spectra which rise as steeply as this are very rare so the vast majority of the 10C sources in the WSRT map are detectable – in fact, all but one of the sources in the complete 10C catalogue are detected in the WSRT map. We therefore define the sample as all 10C sources in the complete catalogue in the OM2008, BI2006 or WSRT deep survey areas. This sample contains 96 sources and accurate positions and spectral index information are therefore available for all but one of the sources. The positions of the sources in the sample are shown in Fig. \[fig:sampleW\]. This 