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The Radius of PSR J0437–4715 from NICER Data

  • Authors: M. C. Miller, A. J. Dittmann, I. M. Holt, F. K. Lamb, C. Chirenti, Z. Arzoumanian, J. Berteaud, S. Bogdanov, K. C. Gendreau, W. C. G. Ho, S. M. Morsink, P. S. Ray, R. A. Remillard, Z. Wadiasingh, M. T. Wolff

M. C. Miller et al 2026 The Astrophysical Journal Letters 1000 .

  • Provider: AAS Journals

Caption: Figure 5.

Mass and radius posteriors, using our best fit to the data of our model with three uniform-temperature circular spots plus a modulated power law—i.e., our Model 5. The dotted lines show the priors. The approximate upper diagonal boundary in the mass–radius plot corresponds to our c2Re/(GM) = 8 prior upper limit, whereas the approximate lower boundary is set by the likelihood rather than by our prior c2Re/(GM) = 3.2 lower limit. The mass posterior is single-peaked and is shifted only slightly from the tight prior given by radio observations, whereas the radius posterior is bimodal (with a larger mode at higher radii).

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