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A Detailed X-Ray Investigation of PSR J2021+4026 and the γ-Cygni Supernova Remnant

  • Authors: C. Y. Hui, K. A. Seo, L. C. C. Lin, R. H. H. Huang, C. P. Hu, J. H. K. Wu, L. Trepl, J. Takata, Y. Wang, Y. Chou, K. S. Cheng, and A. K. H. Kong

Hui et al. 2015 The Astrophysical Journal 799 76.

  • Provider: AAS Journals

Caption: Figure 5.

Pulsation and quiescent stage labeled by the pulse profile of PSR J2021+4026 (0.7–2 keV) as observed by the XMM-Newton/PN camera. The obtained light curve was folded with a spin frequency of 3.768995206 Hz. Two rotation cycles are shown for clarity. Error bars indicate the 1σ uncertainty. The gray-shaded regions and the blue-shaded regions illustrate the off-pulse phase (i.e., DC level) and the on-pulse phase, respectively. The pulsed spectrum was obtained by subtracting the DC level from the source spectrum extracted from the on-pulse phase interval.

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