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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 4.

X-ray brightness profile in the energy band of 0.3–8 keV along the orientation of the PWN associated with PSR J2021+4026 as observed by Chandra ACIS-S3 CCD (see Figure 3). The insets show the bins used in computing the profile. Each bin has a size of 1'' × 10''. The average background level and its 1σ deviation are indicated by horizontal lines that were calculated by sampling from the source-free regions within a 2′ × 2′ field around the pulsar.

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