Fig. D.1.
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EW of the UFO as a function of the 3-10 keV observed flux for the time-resolved spectra (T1-T5) of IRAS 13224-3809. The lack of correlation between the two quantities is directly visualized here, in contrast to the work of Parker et al. (2017), Pinto et al. (2018). The dashed line represents the best-fit anticorrelation reported in Parker et al. (2017) for comparison.
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