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

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arxiv 1109.1590 v1 pith:TNNSOCQ3 submitted 2011-09-07 astro-ph.HE astro-ph.GA

D. Parent , M. Kerr , P. R. Den Hartog , M. G. Baring , M. E. DeCesar , C. M. Espinoza , E. V. Gotthelf , A. K. Harding
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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. Keith M. Kramer A. G. Lyne R. N. Manchester A. Noutsos A. Possenti D. A. Smith
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classification astro-ph.HEastro-ph.GA
keywords emissiongamma-rayj1119-6127pulsarsareaenergeticfermifield
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We report the detection of gamma-ray pulsations from the high-magnetic-field rotation-powered pulsar PSR J1119-6127 using data from the Fermi Large Area Telescope. The gamma-ray light curve of PSR J1119-6127 shows a single, wide peak offset from the radio peak by 0.43 pm 0.02 in phase. Spectral analysis suggests a power law of index 1.0 pm 0.3 with an energy cut-off at 0.8 pm 0.2 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 gamma-ray emitting zone are apparently similar to those of typical young pulsars. Additionally, we present upper limits on the \gam-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.

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