Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· arXiv e-print (arXiv:astro-ph/9901262)
· References in the article
· Citations to the Article (54) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (21)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
SNR G320.4-01.2 and PSR B1509-58: new radio observations of a complex interacting system
Authors:
Gaensler, B. M.; Brazier, K. T. S.; Manchester, R. N.; Johnston, S.; Green, A. J.
Affiliation:
AA(Astrophysics Department, School of Physics A29, University of Sydney, NSW 2006, Australia ), AB(Department of Physics, University of Durham, South Road, Durham DH1 3LE ), AC(Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia ), AD(Research Centre for Theoretical Astrophysics, University of Sydney, NSW 2006, Australia ), AE(Astrophysics Department, School of Physics A29, University of Sydney, NSW 2006, Australia )
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 305, Issue 3, pp. 724-736. (MNRAS Homepage)
Publication Date:
05/1999
Origin:
MNRAS
MNRAS Keywords:
SHOCK WAVES, PULSARS: INDIVIDUAL: B1509-58, ISM: INDIVIDUAL: G320.4-01.2, ISM: INDIVIDUAL: RCW 89, ISM: JETS AND OUTFLOWS, RADIO CONTINUUM: ISM
DOI:
10.1046/j.1365-8711.1999.02500.x
Bibliographic Code:
1999MNRAS.305..724G

Abstract

We describe radio continuum and spectral-line observations of the source G320.4-01.2 (MSH 15-52) and the coincident young pulsar B1509-58 made with the Australia Telescope Compact Array. Based on a comparison between X-ray and radio observations, we argue that the two main radio components of G320.4-01.2 are a single supernova remnant (SNR), which H I absorption indicates is at a distance of 5.2 +/- 1.4 kpc. A high-resolution correspondence between radio and X-rays argues that the pulsar is interacting with the SNR via an opposed pair of collimated outflows. The outflow itself is seen as an elongated X-ray feature surrounded by a highly polarized radio sheath, while the interaction with the SNR manifests itself as a ring of radio/X-ray knots within the optical nebula RCW 89. We reject the hypothesis that the pulsar outflow powers the entire RCW 89 region. SNR G320.4-01.2 and PSR B1509-58 agree in distance and in rotation measure, and appear to be interacting. We thus conclude that the two objects are associated and have an age of 1700 yr. We propose that the SNR resulted from a high-energy or low-mass supernova that occurred near the edge of an elongated cavity. Such a model can account for the bilateral appearance of the SNR, its large apparent age, the significant offset of the pulsar from the centre of the SNR and the faintness of the pulsar-powered nebula at radio wavelengths.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints