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Title:
The X-Ray Structure of the Pulsar Bow Shock G189.22+2.90 in the Supernova Remnant IC 443
Authors:
Gaensler, B. M.; Chatterjee, S.; Slane, P. O.; van der Swaluw, E.; Camilo, F.; Hughes, J. P.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; .; Alfred P. Sloan Research Fellow.; Current address: School of Physics, A29, University of Sydney, NSW 2006, Australia.), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; .; Jansky Fellow, National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903.), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; .), AD(Royal Netherlands Meteorological Institute (KNMI), P.O. Box 201, 3730 AE De Bilt, Netherlands.), AE(Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027.), AF(Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854.)
Publication:
The Astrophysical Journal, Volume 648, Issue 2, pp. 1037-1042. (ApJ Homepage)
Publication Date:
09/2006
Origin:
UCP
ApJ Keywords:
ISM: individual (G189.22+2.90), ISM: Individual: Alphanumeric: IC 443, Stars: Pulsars: Individual: Alphanumeric: CXOU J061705.3+222127, Stars: Neutron, Stars: Winds, Outflows
DOI:
10.1086/506246
Bibliographic Code:
2006ApJ...648.1037G

Abstract

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 postshock 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 standoff 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-1, 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" north and south of the neutron star.
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