Two models to the Chandra-ACIS, XMM-Newton-EPIC pn, and Suzaku-XIS/PIN data used to explain the change in the 2–10 keV spectral shape of F05189–2524: (top) change in the absorbing column alters the spectral shape of the source, and (bottom) the AGN has switched off and has left behind a residual reflection component (see Section 5.1 for details). The response from each detector is folded in with the data. The horizontal axis is energy in the observer's frame. The cross-normalization factor is assumed to be unity for XMM-Newton and Chandra with respect to Suzaku-XIS0. Both models have comparable reduced χ ² values (1.27 for 503 dof vs. 1.30 for 502 dof) and appear to fit the overall 0.5–10 keV spectrum well. Neither model can be ruled out by the data. Table 4 lists the results from this modeling.