PARENT, D.; KERR, M.; R. DEN HARTOG, P.; G. BARING, M.; E. DECESAR, M.; M. ESPINOZA, C.; V. GOTTHELF, E.; K. HARDING, A.; JOHNSTON, S.; M. KASPI, V.; LIVINGSTONE, M.; W. ROMANI, R.; W. STAPPERS, B.; WATTERS, K.; WELTEVREDE, P.; A. ABDO, A.; BURGAY, M.; CAMILO, F.; A. CRAIG, H.; C. C. FREIRE, P.; GIORDANO, F.; GUILLEMOT, L.; HOBBS, G.; KEITH, M.; KRAMER, M.; G. LYNE, A.; N. MANCHESTER, R.; NOUTSOS, A.; POSSENTI, A.; SMITH, David Stanley

doi:10.1088/0004-637X/743/2/170

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The Astrophysical Journal. 2011, vol. 743, p. 170

American Astronomical Society

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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 −0.5 GeV. 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.< Réduire

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Observations of Energetic High Magnetic Field Pulsars with the Fermi Large Area Telescope

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