Comparison of Fe Kα emission and molecular line emission. Top panel: median of the Sgr A complex emission in the Fe Kα 6.4 keV line in the period 2000–2024. The white cross marks the position of Sgr A^⋆. Contours are computed from the N₂H⁺ line intensity, obtained with the MOPRA telescope, integrated over [−30; 80] km s⁻¹ range of velocities (Jones et al. 2012). Contour lines refer to 20, 30, 40, 50, 60, and 70 K km s⁻¹. The central strong emission, encompassing Sgr A^⋆, not associated with molecular clouds, is the supernova remnant Sgr A east (Maeda et al. 2002). Bottom panel: MOPRA longitude–velocity diagram of the same region above. The latitude has been integrated over the [−0.193; 0.169] deg range.