Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (33) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
G27.4+0.0: A galactic supernova remnant with a central compact source
Authors:
Kriss, G. A.; Becker, R. H.; Helfand, D. J.; Canizares, C. R.
Affiliation:
AA(Michigan, University, Ann Arbor, MI; MIT, Cambridge, MA), AB(Virginia Polytechnic Institute and State University, Blacksburg, VA), AC(Columbia, University, New York, NY), AD(MIT, Cambridge, MA)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 288, Jan. 15, 1985, p. 703-706. (ApJ Homepage)
Publication Date:
01/1985
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
NEBULAE, RADIO ASTRONOMY, SUPERNOVA REMNANTS, X RAY SOURCES, HEAO 2, RADIO SPECTRA
DOI:
10.1086/162836
Bibliographic Code:
1985ApJ...288..703K

Abstract

High-resolution X-ray and radio images of the galactic supernova remnant G27.4+0.0 are presented. The X-ray image reveals a centrally located compact source of emission which accounts for 25 percent + or - 2 percent of the emission. The rest of the emission is found in diffuse patches defining a circle of diameter 4 arc min. The radio image is an incomplete shell of comparable diameter with no apparent counterpart to the compact X-ray source. The X-ray luminosity of the supernova remmant implied by the distance of 26 kpc inferred from the Sigma-D relationship exceeds that of any known remnant. This fact, plus the relatively low X-ray absorption, suggests that the remnant is substantially closer than 26 kpc. No X-ray variability of the central source has been detected to a level of 50 percent on time scales of about 1 year, and no periodicity in the range 0.0001-100 Hz to a limit of 16 percent was detected. If G27.4 +0.0 is within a few kiloparsecs, the central source is most likely to be an accretion-powered X-ray binary.

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