Separating cluster soft X-ray emission into its main sources, for four clusters in TNG-Cluster. We break down the total soft X-ray emission (Total) of an example cluster into its main components: gas that is gravitationally bound to the main halo, i.e., brightest central galaxy (BCG), and gas bound to the satellite galaxies (Satellites). Here, satellites are all galaxies besides the BCG that lie within the field of view of the image 3 R_200c × 3 R_200c. We include the haloID and mass $M_{200\mathrm{c}}^{\mathrm{host}}$ in units of [log₁₀ M_⊙] in the lower left in the Total image, and the soft X-ray luminosity $L_{0.5-2.0\mathrm{keV}}^{<1.5R_{200\mathrm{c}}}$ within a projected aperture 1.5 R_200c in units of [log₁₀ erg s⁻¹] in the top right of each panel. We compute the fractional contribution from satellites to the total soft X-ray emission (Satellites/Total), and include both the total soft X-ray contribution from satellites and the mean satellite contribution per pixel in the upper right corner. In all panels the circles denote R_200c. The satellite contributions vary from halo-to-halo, but in general satellites contribute ∼10% of the total soft X-ray flux within ≲1.5 R_200c of the clusters.