Figure 2 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 2.

Folded profiles of PSR J0437–4715 (top left), PSR J0030+0451 (top right), PSR J1231−1411 (bottom left), and PSR J2124−3358 (bottom right). In all instances, phase zero is determined by the radio ephemeris used for event folding. The upper panel for each MSP shows the previous best X-ray profile obtained with XMM-Newton EPIC-pn, with the exception of PSR J1231−1411 for which no prior profile exists. The gray bands mark the phase intervals used for the phase-selected spectroscopy described in Section 8. Two rotational cycles are shown for clarity.

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