tokens: because of missing short spacings. There can be small-scale structure in Stokes Q and U that the interferometer detects, and that can in principle become visible as a component in the Faraday depth spectrum. These are sometimes called Faraday ghosts and are independent of position on the sky (e.g. Shukurov Berkhuijsen 2003 ). Oppermann et al. ( 2012 , 2015 ) have created a map of the smoothly varying Galactic Faraday component, φ gal , by utilizing all-sky Faraday RMs of compact background sources from the literature. We list φ gal at the locations of each of our targets in Table 5 . The effect of the Galactic ISM on an extragalactic source is mainly as a foreground Faraday-rotating screen. The correction for this effect is to subtract φ gal from detected components. In this work, we note that this effect does exist and has possibly affected our measurements but we do not correct for it as it is not adequately constrained. In an effort to analyse Faraday complexity introduced by the ionosphere at the different observation epochs, we look for rotation in the polarization angle (χ) as a function of time. This we do by producing full Stokes images for each scan of the phase calibrator for each epoch. We then restrict our analysis to those scans that have Stokes V flux and p 0 that are below the leakage, and also Stokes I that is above 3σ. We then analyse the resulting q, u , and χ as functions of scan, i.e time. However, the resulting images prove to be too noisy to lead to a conclusion on ionospheric effects. Typical Faraday RM variations from the ionosphere are up to ∼1 rad m −2 . Typical variations are of order 1 rad at 1 m wavelength as χ(λ 2 ) ∼ λ 2 . Variations of this order are seen at 327 MHz at the VLA (Erickson et al. 2001 ). At our lowest frequency even a 90° change at 327 MHz scales to only about 6° at 1300 MHz, and at 1900 MHz. This is small enough to ignore. Note also that it is only the time variation during an epoch that will affect the observations. A constant offset from the ionosphere will be accounted for by the calibration. In the absence of an absolute polarization calibrator, the solution is referenced to the mean feed position angle that is not expected to change as it is hardwired into the instrument. We therefore conclude that the expected ionospheric rotation is negligible and thus not corrected. 4 DISCUSSION Our RM Synthesis analysis shows Faraday complexity, of varying degrees, in four of the six sources in our KAT-7 sample. The most polarized source, J0240−231, displays the most complex Faraday spectrum with several emission components (see Fig. 3a and Table 5 ). The presence of Faraday thick components can be seen in the Faraday spectrum as well. Our analysis clearly resolves this complex spectrum both near the main peak and the smaller peaks. This source also shows the most rapidly changing polarized intensity that depolarizes toward larger wavelengths (see the bottom panel of Fig. 2a ). The behaviour of q
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