Chandra Detection of a Pulsar Wind Nebula Associated with Supernova Remnant 3C 396

Details Chandra Detection of a Pulsar Wind Nebula Associated with Supernova Remnant 3C 396 Chandra Detection of a Pulsar Wind Nebula Associated with Supernova Remnant 3C 396

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...592l..45o&link_type=abstract

The Astrophysical Journal, Volume 592, Issue 1, pp. L45-L48.

Astronomy and Astrophysics

Astronomy

11

Ism: Individual: Alphanumeric: G39.2-0.3, Stars: Pulsars: General, Stars: Neutron, Ism: Supernova Remnants

Scientific paper

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)×1022 cm-2, Γ=1.5+/-0.3] we derive an unabsorbed X-ray flux of SX=1.62×10-12 ergs cm-2 s-1, and from this we estimate the spin-down power of the neutron star to be E=7.2×1036 ergs 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.

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