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)
· arXiv e-print (arXiv:astro-ph/0110218)
· References in the article
· Citations to the Article (10) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (3)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The Interstellar Medium around the Supernova Remnant G320.4-1.2
Authors:
Dubner, G. M.; Gaensler, B. M.; Giacani, E. B.; Goss, W. M.; Green, A. J.
Affiliation:
AA(Instituto de Astronomía y Física del Espacio (CONICET, UBA), C.C. 67, 1428 Buenos Aires, Argentina; .; Member of the Carrera del Investigador Científico of CONICET, Argentina.), AB(Center for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139.; Hubble Fellow.; Current address: Harvard-Smithonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.), AC(Instituto de Astronomía y Física del Espacio (CONICET, UBA), C.C. 67, 1428 Buenos Aires, Argentina; .; Member of the Carrera del Investigador Científico of CONICET, Argentina.), AD(National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801.), AE(School of Physics, University of Sydney, A28, NSW 2006, Australia.)
Publication:
The Astronomical Journal, Volume 123, Issue 1, pp. 337-345. (AJ Homepage)
Publication Date:
01/2002
Origin:
UCP
AJ Keywords:
ISM: individual (G320.4-1.2), ISM: individual (RCW 89), ISM: Structure, pulsars: individual (B1509-58), ISM: Supernova Remnants
DOI:
10.1086/324736
Bibliographic Code:
2002AJ....123..337D

Abstract

Using the Australia Telescope Compact Array, we have carried out a survey of the H I emission in the direction of the barrel-shaped supernova remnant (SNR) G320.4-1.2 (MSH 15-52) and its associated young pulsar B1509-58. The angular resolution of the data is 4.0′×2.7′, and the rms noise is of order 30 mJy beam-1 (~0.5 K). The H I observations indicate that the north-northwest radio limb has encountered a dense H I filament (density ~12 cm-3) at the same LSR velocity as that of the SNR (VLSR~-68 km s-1). This H I concentration would be responsible for the flattened shape of the northwestern lobe of G320.4-1.2 and for the formation of the radio-optical-X-ray nebula RCW 89. The emission associated with the bright knots in the interior of RCW 89 can be explained as arising from the interaction between the collimated relativistic outflow from the pulsar and the denser part of this H I filament (density ~15 cm-3). The south-southeastern half of the SNR, on the other hand, seems to have rapidly expanded across a lower density environment (density ~0.4 cm-3). The H I data also reveal an unusual H I feature aligned with a collimated outflow generated by the pulsar, suggestive of association with the SNR. The anomalous kinematical velocity of this feature (VLSR~15 km s-1), however, is difficult to explain.
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