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/0211374)
· References in the article
· Citations to the Article (3) (Citation History)
· Refereed Citations to the Article
· Associated Articles
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
Erratum: The effect of HII regions on rotation measure of pulsars
Authors:
Mitra, D.; Wielebinski, R.; Kramer, M.; Jessner, A.
Affiliation:
AA(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), AB(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), AC(University of Manchester, Jodrell Bank Observatory, Macclesfield SK11 9DL, UK), AD(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany)
Publication:
Astronomy and Astrophysics, v.403, p.585 (2003) (A&A Homepage)
Publication Date:
05/2003
Origin:
A&A
Astronomy Keywords:
errata, addenda, Galaxy: structure, magnetic fields, ISM: HII regions, stars: pulsars: general
DOI:
10.1051/0004-6361:20030425
Bibliographic Code:
2003A&A...403..585M

Abstract

We have obtained new rotation measure for 11 pulsars observed with the Effelsberg 100-m radio telescope, in the direction of the Perseus arm. Using a combination of 34 published and the 11 newly measured pulsar rotation measures we study the magnetic field structure towards the Perseus arm. We find that two pulsars towards l$\sim$ 149$^{\circ}$ (Region 1) and four pulsars towards l$\sim113^{\circ}$ (Region 2) lie behind HII regions which seriously affects the pulsar rotation measures. The rotation measure of PSR J2337+6151 seem to be affected by its passage through the supernova remnant G114.3+0.3. For Region 1, we are able to constrain the random component of the magnetic field to $5.7\mu$G. For the large-scale component of the Galactic magnetic field we determine a field strength of $1.7\pm1.0\mu$G. This average field is constant on Galactic scales lying within the Galactic longitude range of $85^{\circ} <$ l $ < 240^{\circ}$ and we find no evidence for large scale field reversal upto 5-6 kpc. We highlight the great importance to include the effects of foreground emission in any systematic study.

Associated Articles

Main Paper     Erratum    


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