Top left panel: Diffuse emission as observed by eROSITA within the eFEDS field during e12, fitted with a three-component model (LHB-CGM-CXB in Table 2). The red, blue, magenta, and black solid lines show the contribution from the local hot bubble, circumgalactic medium, cosmic X-ray background, and instrumental background, respectively. The dotted lines show the various contributions to the instrumental background. Top right panel: Same as top left panel, once the contribution from SWCX is added to the model (LHB-CGM-CXB-SWCX). The cyan line shows the contribution due to SWCX. Central left panel: The addition of the emission from the Galactic corona (solid green) significantly improves the fit (LHB-CGM-Coro-CXB). However, significant positive residuals (at the position of the vertical dashed lines) remain at the energy of the blue wing of the very prominent O VII emission line as well as negative residuals on its red wing. Central right panel: Same as central left panel, with the addition of the SWCX component (LHB-CGM-CXB-Coro-SWCX model). Bottom left panel: The addition of a significantly different energy shift applied to the best fit model of each camera reduces the residuals around the O VII emission line (shift-LHB-CGM-Coro-CXB). Bottom right panel: Same as bottom left panel, with the addition of the SWCX component (shift-LHB-CGM-CXB-Coro-SWCX model).