The Vela Pulsar: Results from the First Year of Fermi LAT Observations

A. A. Abdo , Markus Ackermann , Marco Ajello , A. Allafort , W. B. Atwood , Luca Baldini , Jean Ballet (1) , Guido Barbiellini , M. G. Baring , D. Bastieri , B. M. Baughman , K. Bechtol , R. Bellazzini (1) , B. Berenji , R. D. Blandford , E. D. Bloom , E. Bonamente , A. W. Borgland , A. Bouvier , J. Bregeon (2) , A. Brez , M. Brigida , Pascal Bruel (3) , T. H. Burnett , S. Buson , G. A. Caliandro , R. A. Cameron , P. A. Caraveo , S. Carrigan , J. M. Casandjian (1) , C. Cecchi , O. Celik , A. Chekhtman , C. C. Cheung , J. Chiang , S. Ciprini , R. Claus , J. Cohen-Tanugi (4) , J. Conrad , C. D. Dermer , A. de Luca , F. de Palma , M. Dormody , E. Do Couto E Silva , P. S. Drell , R. Dubois , D. Dumora (2) , C. Farnier (4) , C. Favuzzi , S. J. Fegan (3) , W. B. Focke , P. Fortin (3) , M. Frailis , Y. Fukazawa , S. Funk , P. Fusco , F. Gargano , D. Gasparrini , N. Gehrels , S. Germani , G. Giavitto , B. Giebels (3) , N. Giglietto , F. Giordano , T. Glanzman , G. Godfrey , I. A. Grenier (1) , M.-H. Grondin (2) , J. E. Grove , L. Guillemot (2) , S. Guiriec (4) , D. Hadasch , A. K. Harding , E. Hays , G. Hobbs , D. Horan (3) , R. E. Hughes , M. S. Jackson , G. Johannesson , A. S. Johnson , T. J. Johnson , W. N. Johnson , T. Kamae , H. Katagiri , J. Kataoka , N. Kawai , M. Kerr , Jürgen Knödlseder (5) , M. Kuss , J. Lande , L. Latronico , S.-H. Lee , M. Lemoine-Goumard (2) , M. Llena Garde , F. Longo , F. Loparco , B. Lott (2) , M. N. Lovellette , P. Lubrano , A. Makeev , R. N. Manchester , M. Marelli , M. N. Mazziotta , W. Mcconville , J. E. Mcenery , S. Mcglynn , C. Meurer , P. F. Michelson , W. Mitthumsiri , T. Mizuno , A. A. Moiseev , C. Monte , M. E. Monzani , A. Morselli , I. V. Moskalenko , S. Murgia , T. Nakamori , P. L. Nolan , J. P. Norris , A. Noutsos , E. Nuss (4) , T. Ohsugi , N. Omodei , E. Orlando , J. F. Ormes , M. Ozaki , D. Paneque , J. H. Panetta , D. Parent (2) , V. Pelassa (4) , M. Pepe , M. Pesce-Rollins , M. Pierbattista (1) , F. Piron (4) , T.A. Porter , S. Raino , R. Rando , P. S. Ray , M. Razzano , A. Reimer , O. Reimer , T. Reposeur (2) , S. Ritz , L. S. Rochester , A. Y. Rodriguez , R. W. Romani , M. Roth , F. Ryde , H. F.-W. Sadrozinski , A. Sander , P. M. Saz Parkinson , C. Sgro (3) , E. J. Siskind , David Stanley Smith (2) , P. D. Smith , G. Spandre , P. Spinelli , Jean-Luc Starck (1) , M. S. Strickman , D. J. Suson , H. Takahashi , T. Takahashi , T. Tanaka , J. B. Thayer , J. G. Thayer , D. J. Thompson , L. Tibaldo (1) , D. F. Torres , G. Tosti , A. Tramacere , T. L. Usher , A. van Etten , V. Vasileiou , C. Venter , 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 AIM (UMR7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
2 CENBG - Centre d'Etudes Nucléaires de Bordeaux Gradignan
3 LLR - Laboratoire Leprince-Ringuet
4 LPTA - Laboratoire de Physique Théorique et Astroparticules
5 CESR - Centre d'étude spatiale des rayonnements

We report on analysis of timing and spectroscopy of the Vela pulsar using eleven months of observations with the Large Area Telescope on the Fermi Gamma-Ray Space Telescope. The intrinsic brightness of Vela at GeV energies combined with the angular resolution and sensitivity of the LAT allow us to make the most detailed study to date of the energy-dependent light curves and phase-resolved spectra, using a LAT-derived timing model. The light curve consists of two peaks (P1 and P2) connected by bridge emission containing a third peak (P3). We have confirmed the strong decrease of the P1/P2 ratio with increasing energy seen with EGRET and previous Fermi LAT data, and observe that P1 disappears above 20 GeV. The increase with energy of the mean phase of the P3 component can be followed with much greater detail, showing that P3 and P2 are present up to the highest energies of pulsation. We find significant pulsed emission at phases outside the main profile, indicating that magnetospheric emission exists over 80% of the pulsar period. With increased high-energy counts the phase-averaged spectrum is seen to depart from a power- law with simple exponential cutoff, and is better fit with a more gradual cutoff. The spectra in fixed-count phase bins are well fit with power-laws with exponential cutoffs, revealing a strong and complex phase dependence of the cutoff energy, especially in the peaks. By combining these results with predictions of the outer magnetosphere models that map emission characteristics to phase, it will be possible to probe the particle acceleration and the structure of the pulsar magnetosphere with unprecedented detail.

Mots clés: pulsars: general; stars: neutron

Domaines: Phénomènes cosmiques de haute energie [astro-ph.HE]; Phénomènes cosmiques de haute energie [astro-ph.HE]; Astrophysique galactique [astro-ph.GA]; Astrophysique galactique [astro-ph.GA]

A. A. Abdo, Markus Ackermann, Marco Ajello, A. Allafort, W. B. Atwood, et al.. The Vela Pulsar: Results from the First Year of Fermi LAT Observations. The Astrophysical Journal, 2010, 713, pp.154-165. ⟨10.1088/0004-637X/713/1/154⟩. ⟨in2p3-00482639⟩