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Chandra Observations of the Pulsar Wind Nebula in Supernova Remnant G0.9+0.1

B. M. Gaensler et al 2001 ApJ 556 L107-L111   doi: 10.1086/322982  Help

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B. M. Gaensler1,2, M. J. Pivovaroff1,3 and G. P. Garmire4
1 Center for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139
2 Hubble Fellow
3 Current address: Therma-Wave Inc., 1250 Reliance Way, Fremont, CA 94539
4 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802
E-mail: bmg@space.mit.edu

ABSTRACT. We present observations with the Chandra X-Ray Observatory of the pulsar wind nebula (PWN) within the supernova remnant G0.9+0.1. At Chandra's high resolution, the PWN has a clear axial symmetry; a faint X-ray point source lying along the symmetry axis possibly corresponds to the pulsar itself. We argue that the nebular morphology can be explained in terms of a torus of emission in the pulsar's equatorial plane and a jet directed along the pulsar spin axis, as is seen in the X-ray nebulae powered by other young pulsars. A bright clump of emission within the PWN breaks the axisymmetry and may correspond to an intermediate-latitude feature in the pulsar wind.

Subject headings: ISM: individual (G0.9+0.1); pulsars: general; stars: winds, outflows; supernova remnants

Print publication: Issue 2 (2001 August 1)
Received 2001 May 14, accepted for publication 2001 June 26
Published 2001 July 16

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