Observations of energetic high magnetic field pulsars with the Fermi large area telescope

Research output: Contribution to journalArticle

  • External authors:
  • D. Parent
  • M. Kerr
  • P. R. Den Hartog
  • M. G. Baring
  • M. E. DeCesar
  • C. M. Espinoza
  • E. V. Gotthelf
  • A. K. Harding
  • S. Johnston
  • V. M. Kaspi
  • M. Livingstone
  • R. W. Romani
  • B. W. Stappers
  • K. Watters
  • P. Weltevrede
  • A. A. Abdo
  • M. Burgay
  • F. Camilo
  • H. A. Craig
  • P. C C Freire
  • F. Giordano
  • L. Guillemot
  • G. Hobbs
  • M. Kramer
  • A. G. Lyne
  • R. N. Manchester
  • A. Noutsos
  • A. Possenti
  • D. A. Smith

Abstract

We report the detection of γ-ray pulsations from the high-magnetic-field rotation-powered pulsar PSR J1119-6127 using data from the Fermi Large Area Telescope. The γ-ray light curve of PSR J1119-6127 shows a single, wide peak offset from the radio peak by 0.43 0.02 in phase. Spectral analysis suggests a power law of index 1.0 0.3+0.4-0.2 with an energy cutoff at 0.8 0.2+2.0-0.5GeV. The first uncertainty is statistical and the second is systematic. We discuss the emission models of PSR J1119-6127 and demonstrate that despite the object's high surface magnetic field - near that of magnetars - the field strength and structure in the γ-ray emitting zone are apparently similar to those of typical young pulsars. Additionally, we present upper limits on the γ-ray pulsed emission for the magnetically active PSR J1846-0258 in the supernova remnant Kesteven 75 and two other energetic high-B pulsars, PSRs J1718-3718 and J1734-3333. We explore possible explanations for the non-detection of these three objects, including peculiarities in their emission geometry. © 2011 The American Astronomical Society. All rights reserved.

Bibliographical metadata

Original languageEnglish
Article number170
JournalAstrophysical Journal
Volume743
Issue number2
DOIs
Publication statusPublished - 20 Dec 2011