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/0305497)
· On-line Data
· References in the article
· Citations to the Article (26) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (8)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Chandra Detection of the High Magnetic Field Radio Pulsar J1119-6127in the Supernova Remnant G292.2-0.5
Authors:
Gonzalez, Marjorie; Safi-Harb, Samar
Affiliation:
AA(Physics and Astronomy Department, University of Manitoba, Winnipeg, MB R3T 2N2, Canada; , . ; NSERC PGSA Fellow.), AB(Physics and Astronomy Department, University of Manitoba, Winnipeg, MB R3T 2N2, Canada; , . ; NSERC UFA Fellow.)
Publication:
The Astrophysical Journal, Volume 591, Issue 2, pp. L143-L146. (ApJL Homepage)
Publication Date:
07/2003
Origin:
UCP
ApJ Keywords:
ISM: Individual: Alphanumeric: G292.2-0.5, Stars: Pulsars: Individual: Alphanumeric: PSR J1119-6127, pulsars: individual (AX J1119.1-6128.5), ISM: Supernova Remnants, X-Rays: ISM
DOI:
10.1086/377070
Bibliographic Code:
2003ApJ...591L.143G

Abstract

We report the Chandra Advanced CCD Imaging Spectrometer detection of the X-ray counterpart of the high magnetic field, ~1600 yr old, 407 ms radio pulsar J1119-6127 associated with the supernova remnant G292.2-0.5. The powerful imaging capability of Chandra also unveiled, for the first time, a faint 3''×6'' pulsar wind nebula (PWN) at energies above ~1.2 keV. The X-ray emission from the pulsar and its associated nebula is well described by an absorbed power law model with a photon index Γ=2.2+0.6-0.3. The corresponding 0.5-10 keV unabsorbed X-ray luminosity is (5.5+10-3.3)×1032 ergs s-1 (at 6 kpc). When compared to two other pulsars with similar spin and magnetic properties, J1119-6127 stands out as being the least efficient at turning rotational kinetic energy into X-ray emission. This study shows that high magnetic field radio pulsars can be significant X-ray emitters, and Chandra is needed to study the emission properties of the pulsars and associated faint PWNs.
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