We present a 100 ks observation of the Galactic supernova remnant 3C 396 (G39.2-0.3) with the Chandra X-Ray Observatory that we compare with a 20 cm map of the remnant from the Very Large Array. In the Chandra images, a nonthermal nebula containing an embedded pointlike source is apparent near the center of the remnant that we interpret as a synchrotron pulsar wind nebula surrounding a yet undetected pulsar. From the 2-10 keV spectrum for the nebula [NH= (5.3 ± 0.9) × 1022cm-2, Γ = 1.5 ± 0.3] we derive an unabsorbed X-ray flux of Sx= 1.62 × 10-12ergs cm-2s-1, and from this we estimate the spin-down power of the neutron star to be Ė = 7.2 × 1036ergs s-1. The central nebula is morphologically complex, showing bent, extended structure. The radio and X-ray shells of the remnant correlate poorly on large scales, particularly on the eastern half of the remnant, which appears very faint in X-ray images. At both radio and X-ray wavelengths, the western half of the remnant is substantially brighter than the eastern half.
CITATION STYLE
Olbert, C. M., Keohane, J. W., Arnaud, K. A., Dyer, K. K., Reynolds, S. P., & Safi-Harb, S. (2003). Chandra Detection of a Pulsar Wind Nebula Associated with Supernova Remnant 3C 396. The Astrophysical Journal, 592(1), L45–L48. https://doi.org/10.1086/377348
Mendeley helps you to discover research relevant for your work.