Image Details
Caption: Figure 3.
Phase-channel residuals for the best fit to the data of our model with three uniform-temperature circular spots plus a modulated power law, over the full set of 32 uniformly spaced rotational phases and NICER PI channels 30–299 inclusive. Here, for a phase-channel bin i, if the data have di counts and the model predicts mi counts, we define ﹩\chi \equiv ({m}_{i}-{d}_{i})/\sqrt{{m}_{i}}﹩. In addition to the fit having an overall acceptable χ2/dof = 8335.00/8345 (for which the probability of this χ2 or higher for a correct model is 53%), there are no patterns visible and no individual phase-channel bins with an unexpectedly large ∣χ∣. This is a one-way test: our satisfactory fit does not guarantee that the model is correct, but a very low probability would indicate that we would need to look more closely at our model.
© 2026. The Author(s). Published by the American Astronomical Society.