Fig. 2.
Top panel: pulse phase delays as a function of time computed by epoch-folding at a constant frequency ∼400 s and 300 s data intervals of the NuSTAR (left) and the NICER (right) data sets, respectively, after correcting for the best orbital solution. In the same panel we show the best-fit models for each group of data. Bottom panel: residuals in μs with respect to the best-fitting models for the pulse phase delays.
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