Figure 5 from Constraining the Neutron Star Mass–Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set

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Constraining the Neutron Star Mass–Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set

Authors: Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Michael T. Wolff, Deepto Chakrabarty, Wynn C. G. Ho, Matthew Kerr, Frederick K. Lamb, Andrea Lommen, Renee M. Ludlam, Reilly Milburn, Sergio Montano, M. Coleman Miller, Michi Bauböck, Feryal Özel, Dimitrios Psaltis, Ronald A. Remillard, Thomas E. Riley, James F. Steiner, Tod E. Strohmayer, Anna L. Watts, Kent S. Wood, Jesse Zeldes, Teruaki Enoto, Takashi Okajima, James W. Kellogg, Charles Baker, Craig B. Markwardt, Zaven Arzoumanian, and Keith C. Gendreau

2019 The Astrophysical Journal Letters 887 L25.

Provider: AAS Journals

Caption: Figure 5.

Folded NICER XTI profiles from Figure 2 but grouped in 256 (for PSRs J0437−4715 and J0030+0451) or 128 phase bins (for PSRs J1231−1411 and J2124−3358). The solid red lines show the best fit with a model of the profile constructed from the empirical Fourier coefficients, given by Equation (1), of the set of photon phases. The dashed lines show the sinusoids corresponding to the first four harmonic components of the fit (blue, orange, purple, and cyan for the first, second, third, and fourth harmonic, respectively). The bottom panel for each pulsar shows the residuals from the fit.

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