estimate the S/N for the integrated signal per filament with the SKA, where the S/N then depends on the three-dimensional orientation of the filament. Here, we outline which steps will be required to make a detection and how we estimate the noise that can be expected for such an observation with the SKA.\
In this case we consider the two phases of the telescope separately. The first phase of the SKA will consist of the 64 13.5m dishes currently operating as the Karoo Array Telescope (MeerKAT) together with 133 dishes of 15m diameter that will be added to it[^1]. For its second phase, this system will be significantly expanded to a total of 1500 dishes, which will result in an unprecedented sensitivity at these frequencies. The relevant properties of these two arrays that will be used in this study are summarized in Table \[tab:specs\].\

  Parameter                                                       SKA1-Mid                SKA-2
  --------------------------------------------------- -------------------------------- -----------
  Number of dishes, $N_{\rm dish}$                                  197                   1500
  Dish diameter, $D_{\rm dish}$ (m)                    64$\times$13.5 + 133$\times$15      15
  Total collecting area, $A_{\rm tot}$ ($\rm{m}^2$)                32,664                265,071
  System temperature, $T_{\rm sys}$ (K)                              20                    30
  Aperture efficiency, $\epsilon_{\rm ap}$                          0.8                    0.8
  Field of View ($\rm{deg}^2$)                                    $\sim$1                $\sim$1
  Angular resolution (arcsec)                                    $\sim$0.3              $\sim$0.1
  System Equivalent                                                                    
  