The X-ray Structure of the Pulsar Bow Shock G189.22+2.90 in the Supernova Remnant IC 443

Details The X-ray Structure of the Pulsar Bow Shock G189.22+2.90 in the Supernova Remnant IC 443 The X-ray Structure of the Pulsar Bow Shock G189.22+2.90 in the Supernova Remnant IC 443

2006-01-13

arxiv.org/abs/astro-ph/0601304v2

Astrophys.J.648:1037-1042,2006

Astronomy and Astrophysics

Astrophysics

8 pages, including 3 color EPS figure. Expaneded to include new figures, plus discussion of the association between the pulsar

Scientific paper

10.1086/506246

We present a deep observation with the Chandra X-ray Observatory of the neutron star bow shock G189.22+2.90 in the supernova remnant (SNR) IC 443. Our data confirm the cometary morphology and central point source seen previously, but also reveal considerable new structure. Specifically, we find that the X-ray nebula consists of two distinct components: a "tongue" of bright emission close to the neutron star, enveloped by a larger, fainter "tail". We interpret the tongue and tail as delineating the termination shock and the post-shock flow, respectively, as previously identified also in the pulsar bow shock G359.23-0.82 ("the Mouse"). However, for G189.22+2.90 the tongue is much less elongated than for the Mouse, while the tail is much broader. These differences are consistent with the low Mach number, M >~ 2, expected for a neutron star moving through the hot gas in a SNR's interior, supporting the case for a physical association between G189.22+2.90 and IC 443. We resolve the stand-off distance between the star and the head of the bow shock, which allows us to estimate a space velocity for the neutron star of ~230 km/s, independent of distance. We detect thermal emission from the neutron star surface at a temperature of 102 +/- 22 eV, which is consistent with the age of SNR IC 443 for standard neutron star cooling models. We also identify two compact knots of hard emission located 1-2 arcsec north and south of the neutron star.

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