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Title:
Discovery of Pulsed γ-Rays from the Young Radio Pulsar PSR J1028-5819 with the Fermi Large Area Telescope
Authors:
Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Donato, D.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fleury, P.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M.-H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Komin, N.; Kramer, M.; Kuehn, F.; Kuss, M.; Latronico, L.; Lee, S.-H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F.-W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J.-L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Waite, A. P.; Watters, K.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Hobbs, G.; Keith, M.; Manchester, R. N.; Weltevrede, P.
Affiliation:
AA(Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA; National Research Council Research Associate. ), AB(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA ), AC(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, CA 95064, USA), AD(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy), AE(Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d'Astrophysique, CEA Saclay, 91191 Gif sur Yvette, France), AF(Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy; Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy), AG(Rice University, Department of Physics and Astronomy, MS-108, P.O. Box 1892, Houston, TX 77251, USA), AH(Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy; Dipartimento di Fisica "G. Galilei", Università di Padova, I-35131 Padova, Italy), AI(Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA), AJ(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), AK(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy), AL(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), AM(W. W. 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Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy; Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy), FP(Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d'Astrophysique, CEA Saclay, 91191 Gif sur Yvette, France), FQ(Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA), FR(Department of Chemistry and Physics, Purdue University Calumet, Hammond, IN 46323-2094, USA), FS(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), FT(Department of Physical Science and Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima 739-8526, Japan), FU(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), FV(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), FW(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), FX(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), FY(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, CA 95064, USA), FZ(Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy; Dipartimento di Fisica "G. Galilei", Università di Padova, I-35131 Padova, Italy), GA(Institució Catalana de Recerca i Estudis Avançats (ICREA), Barcelona, Spain; Institut de Ciencies de l'Espai (IEEC-CSIC), Campus UAB, 08193 Barcelona, Spain), GB(Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy; Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy), GC(Consorzio Interuniversitario per la Fisica Spaziale (CIFS), I-10133 Torino, Italy; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), GD(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), GE(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), GF(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), GG(Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, BP 44346, F-30128 Toulouse Cedex 4, France), GH(Istituto Nazionale di Fisica Nucleare, Sezione di Roma "Tor Vergata", I-00133 Roma, Italy; Dipartimento di Fisica, Università di Roma "Tor Vergata", I-00133 Roma, Italy), GI(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), GJ(W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305, USA), GK(Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA), GL(School of Pure and Applied Natural Sciences, University of Kalmar, SE-391 82 Kalmar, Sweden; The Oskar Klein Centre for Cosmo Particle Physics, AlbaNova, SE-106 91 Stockholm, Sweden; Department of Physics, Royal Institute of Technology (KTH), AlbaNova, SE-106 91 Stockholm, Sweden), GM(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, CA 95064, USA), GN(Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia), GO(Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia), GP(Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia), GQ(Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia)
Publication:
The Astrophysical Journal Letters, Volume 695, Issue 1, pp. L72-L77 (2009). (ApJL Homepage)
Publication Date:
04/2009
Origin:
IOP
Astronomy Keywords:
pulsars: general, stars: neutron
DOI:
10.1088/0004-637X/695/1/L72
Bibliographic Code:
2009ApJ...695L..72A

Abstract

Radio pulsar PSR J1028-5819 was recently discovered in a high-frequency search (at 3.1 GHz) in the error circle of the Energetic Gamma-Ray Experiment Telescope (EGRET) source 3EG J1027-5817. The spin-down power of this young pulsar is great enough to make it very likely the counterpart for the EGRET source. We report here the discovery of γ-ray pulsations from PSR J1028-5819 in early observations by the Large Area Telescope (LAT) on the Fermi Gamma-Ray Space Telescope. The γ-ray light curve shows two sharp peaks having phase separation of 0.460 ± 0.004, trailing the very narrow radio pulse by 0.200 ± 0.003 in phase, very similar to that of other known γ-ray pulsars. The measured γ-ray flux gives an efficiency for the pulsar of ~10-20% (for outer magnetosphere beam models). No evidence of a surrounding pulsar wind nebula is seen in the current Fermi data but limits on associated emission are weak because the source lies in a crowded region with high background emission. However, the improved angular resolution afforded by the LAT enables the disentanglement of the previous COS-B and EGRET source detections into at least two distinct sources, one of which is now identified as PSR J1028-5819.
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