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/9711331)
· References in the article
· Citations to the Article (15) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (11)
· NED Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Radio continuum and HI observations of the supernova remnant G296.8-00.3
Authors:
Gaensler, B. M.; Manchester, R. N.; Green, A. J.
Affiliation:
AA(Astrophysics Department, School of Physics A29, University of Sydney, NSW 2006, Australia), AB(Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 2121, Australia), AC(Astrophysics Department, School of Physics A29, University of Sydney, NSW 2006, Australia)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 296, Issue 4, pp. 813-823. (MNRAS Homepage)
Publication Date:
06/1998
Origin:
MNRAS
MNRAS Keywords:
SHOCK WAVES, TECHNIQUES: POLARIMETRIC, PULSARS: INDIVIDUAL: J1157-6224, ISM: INDIVIDUAL: G296.8-00.3, SUPERNOVA REMNANTS, RADIO LINES: ISM
DOI:
10.1046/j.1365-8711.1998.01387.x
Bibliographic Code:
1998MNRAS.296..813G

Abstract

We present Australia Telescope Compact Array (ATCA) observations of the supernova remnant (SNR) G296.8-00.3. A 1.3-GHz continuum image shows the remnant to have a complex multi-shelled appearance, with an unusual rectangular strip running through its centre. HI absorption yields a kinematic distance to the remnant of 9.6+/-0.6 kpc, from which we estimate an age in the range (2-10)x10^3 yr. The ATCA's continuum mode allows a measurement of the Faraday rotation across the band, from which we derive a mean rotation measure towards the SNR of 430 rad m^-2. We consider possible explanations for the morphology of G296.8-00.3, and conclude that either it has a biannular structure, as might be produced through interaction with an asymmetric progenitor wind, or its appearance is caused by the effects of the surrounding interstellar medium. We argue that the adjacent pulsar J1157-6224 is at a similar distance to the SNR, but that a physical association is highly unlikely. The pulsar is the only detectable source in the field in circular polarization, suggesting a method for finding pulsars during aperture synthesis.

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