Total intensity (left) and polarised (right) surface brightness images expected from observations in the frequency range of 110–166 MHz and with a spectral resolution of 45 kHz with the SKALOW telescope, smoothed to a resolution of 20″. Red contours represent the 3σ_I, and blue contours the 5σ_P sensitivity expected after 10 h and 100 h. The FWHM is shown in the bottom left of each image. The simulated diffuse radio emission was obtained assuming a magnetic field and a thermal gas density distribution simulated by Xu et al. (2012) and a relativistic electron population in equipartition with the magnetic field (first and third row) and with an energy density equal to 0.3% of the thermal one (second and fourth row); see the text for more details.