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First Look at the High-resolution X-Ray Spectra in the Highly Absorbed High-mass X-Ray Binary IGR J16318−4848 with Chandra

  • Authors: Pragati Pradhan, David P. Huenemoerder, Biswajit Paul, Roberta Amato, Ralf Ballhausen, Claude Canizares, Joel B. Coley, Camille M. Diez, Felix Fürst, Poshak Gandhi, Victoria Grinberg, Sean Gunderson, Richard Ignace, Peter Kretschmar, Maximilian Lorenz, Christian Malacaria, Antonios Manousakis, Silvia Martínez-Núñez, Katja Pottschmidt, Jérôme Rodriguez, Richard E. Rothschild, José M. Torrejón, Bert Vander Meulen, Jörn Wilms

Pragati Pradhan et al 2026 The Astrophysical Journal 1004 .

  • Provider: AAS Journals

Caption: Figure 7.

Radial velocities of the Fe Kα line as a function of orbital phase (with 1σ errors). The velocities were derived from the measured line centroids relative to the Fe Kα1 line at 6.404 keV and after heliocentric corrections, modeled with a sinusoid ﹩{v}_{{\rm{rad}}}(\phi )=K\,\sin (2\pi \,\phi +{\phi }_{0})+{v}_{0}﹩, where K is the semiamplitude, ϕ0 is the phase offset, and v0 is the systemic velocity. The blue line shows the best-fit sinusoidal model, with parameters K = 167 ± 32 km s−1, ϕ0 = (0.55 ± 0.08) π, and v0 = 0.5 ± 23 km s−1. The red dashed line represents a constant fit.

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