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Fermi LAT Observations of the Vela Pulsar

A.A. Abdo Markus Ackermann W. B. Atwood R. Bagagli Luca Baldini Jean Ballet D. L. Band Guido Barbiellini M. G. Baring J. Bartelt D. Bastieri B. M. Baughman K. Bechtol F. Bellardi R. Bellazzini B. Berenji D. Bisello R. D. Blandford E. D. Bloom J. R. Bogart E. Bonamente A. W. Borgland A. Bouvier J. Bregeon A. Brez M. Brigida Pascal Bruel 1 T. H. Burnett G. A. Caliandro R. A. Cameron F. Camilo P. A. Caraveo J. M. Casandjian 2 M. Ceccanti C. Cecchi E. Charles A. Chekhtman C. C. Cheung J. Chiang S. Ciprini R. Claus Ismaël Cognard J. Cohen-Tanugi 3 L. R. Cominsky J. Conrad R. Corbet L. Corucci S. Cutini D. S. Davis M. Deklotz C. D. Dermer A. de Angelis F. de Palma S. W. Digel M. Dormody E. Do Couto E Silva P. S. Drell R. Dubois D. Dumora 4 C. Espinoza C. Farnier 3 C. Favuzzi D. L. Flath P. Fleury 1 W. B. Focke M. Frailis P. C. C. Friere Y. Fukazawa S. Funk P. Fusco F. Gargano D. Gasparrini N. Gehrels S. Germani R. Giannitrapani B. Giebels 1 N. Giglietto F. Giordano T. Glanzman G. Godfrey E. V. Gotthelf I. A. Grenier M.-H. Grondin 4 J. E. Grove L. Guillemot 4 S. Guiriec 3 G. Haller A. K. Harding P. A. Hart R. C. Hartman E. Hays G. Hobbs R. E. Hughes G. J'Ohannesson A. S. Johnson R. P. Johnson T. J. Johnson W. N. Johnson S. Johnston T. Kamae G. Kanbach V. M. Kaspi H. Katagiri J. Kataoka A. Kavelaars N. Kawai H. Kelly M. Kerr B. Kiziltan W. Klamra J. Kn¨o Dlseder 5 M. Kramer F. Kuehn M. Kuss J. Lande D. Landriu 2 L. Latronico B. Lee S.-H. Lee M. Lemoine-Goumard 4 M. Livingstone F. Longo F. Loparco B. Lott 4 M. N. Lovellette P. Lubrano A. G. Lyne G. M. Madejski A. Makeev R. N. Manchester B. Marangelli M. Marelli M. N. Mazziotta J. E. Mcenery S. Mcglynn M. A. Mclaughlin N. Menon C. Meurer P. F. Michelson T. Mineo N. Mirizzi W. Mitthumsiri T. Mizuno A. A. Moiseev M. Mongelli C. Monte M. E. Monzani E. Moretti A. Morselli I. V. Moskalenko S. Murgia T. Nakamori P. L. Nolan A. Noutsos E. Nuss 3 T. Ohsugi N. Omodei E. Orlando J. F. Ormes M. Ozaki A. Paccagnella D. Paneque J. H. Panetta D. Parent 4 M. Pearce M. Pepe M. Perchiazzi M. Pesce-Rollins L. Pieri M. Pinchera F. Piron 3 T.A. Porter S. Rain'O R. Rando S. M. Ransom E. Rapposelli M. Razzano A. Reimer O. Reimer T. Reposeur 4 L. C. Reyes S. Ritz L. S. Rochester A. Y. Rodriguez R. W. Romani M. Roth F. Ryde A. Sacchetti H. F.-W. Sadrozinski N. Saggini D. Sanchez 1 A. Sander P. M. Saz Parkinson K. N. Segal A. Sellerholm C. Sgr'O E. J. Siskind David Stanley Smith 4 P. D. Smith G. Spandre P. Spinelli M. Stamatikos Jean-Luc Starck F. W. Stecker T. E. Stephens M. S. Strickman A. W. Strong D. J. Suson H. Tajima H. Takahashi T. Takahashi T. Tanaka A. Tenze J. B. Thayer J. G. Thayer G. Theureau 6 D. J. Thompson S. E. Thorsett L. Tibaldo O. Tibolla D. F. Torres A. Tramacere M. Turri T. L. Usher L. Vigiani N. Vilchez 5 V. Vitale A. P. Waite P. Wang K. Watters P. Weltevrede B. L. Winer K. S. Wood T. Ylinen M. Ziegler
1 LLR - Laboratoire Leprince-Ringuet
2 AIM (UMR_7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
3 LPTA - Laboratoire de Physique Théorique et Astroparticules
4 CENBG - Centre d'Etudes Nucléaires de Bordeaux Gradignan
5 CESR - Centre d'étude spatiale des rayonnements
6 LPCE - Laboratoire de physique et chimie de l'environnement
Abstract : The Vela pulsar is the brightest persistent source in the GeV sky and thus is the traditional first target for new gamma-ray observatories. We report here on initial Fermi Large Area Telescope observations during verification phase pointed exposure and early sky survey scanning. We have used the Vela signal to verify Fermi timing and angular resolution. The high quality pulse profile, with some 32,400 pulsed photons at E>0.03 GeV, shows new features, including pulse structure as fine as 0.3ms and a distinct third peak, which shifts in phase with energy. We examine the high energy behavior of the pulsed emission; initial spectra suggest a phase-averaged power law index of Gamma=1.51{+0.05/-0.04} with an exponential cut-off at E_c=2.9+/-0.1 GeV. Spectral fits with generalized cut-offs of the form e^{-(E/E_c)^b} require b<1, which is inconsistent with magnetic pair attenuation, and thus favor outer magnetosphere emission models. Finally, we report on upper limits to any unpulsed component, as might be associated with a surrounding synchrotron wind nebula (PWN).
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A.A. Abdo, Markus Ackermann, W. B. Atwood, R. Bagagli, Luca Baldini, et al.. Fermi LAT Observations of the Vela Pulsar. The Astrophysical Journal, American Astronomical Society, 2009, 696, pp.1084-1093. ⟨10.1088/0004-637X/696/2/1084⟩. ⟨in2p3-00378125⟩

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