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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 8.

XMM-Newton EPIC MOS1/2 images of PSRs J0437−4715 (top left), J0030+0451 (top right), J1231−1411 (bottom left), and J2124−3358 (bottom right) and nearby sources marked with blue circles. The large dashed yellow circle indicates the NICER point-spread function with half-power diameter of 6.′2. For PSRs J0437−4715 and J2124−3358, the teal “×” shows the position of the optimal NICER pointing that maximizes the S/N from the pulsar, i.e., minimizes the contamination from surrounding sources. For the other two pulsars, PSRs J0030+0451 and J1231−1411, the optimal pointing distance from the pulsar and the gain in S/N are negligible.

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