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Title:
The Fermi Gamma-Ray Space Telescope Discovers the Pulsar in the Young Galactic Supernova Remnant CTA 1
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.; Blandford, R. D.; Bloom, E. D.; Bogaert, G.; 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.; Carlson, P.; 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.; Cutini, S.; Davis, D. S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Focke, W. B.; 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.; Hartman, R. C.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Kanai, Y.; Kanbach, G.; Katagiri, H.; Kawai, N.; Kerr, M.; Kishishita, T.; Kiziltan, B.; Knödlseder, J.; Kocian, M. L.; Komin, N.; Kuehn, F.; Kuss, M.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Lonjou, V.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mineo, T.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piano, G.; Pieri, L.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; 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; Schalk, T. L.; Sellerholm, A.; 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.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Wang, P.; Watters, K.; Winer, B. L.; Wood, K. S.; Yasuda, H.; Ylinen, T.; Ziegler, M.
Affiliation:
AA(National Research Council Research Associate, National Academy of Sciences, Washington, DC 20001, USA.; Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA.), 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, Santa Cruz, CA 95064, USA.), AD(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), AE(Laboratoire Astrophysique, Interactions, Multi-échelles–Commissariat à l’Énergie Atomique (CEA)–CNRS-Université Paris Diderot, Service d’Astrophysique, CEA Saclay, F-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, Post Office 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. 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.), AN(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.), AO(Laboratoire Leprince-Ringuet, École Polytechnique, CNRS/IN2P3, Palaiseau, France.), AP(Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy.; Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy.), AQ(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.), AR(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), AS(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), AT(Dipartimento di Fisica “M. 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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.), AY(Istituto Nazionale di Astrofisica–Istituto di Astrofisica Spaziale e Fisica Cosmica, I-20133 Milano, Italy.), AZ(Department of Physics, Royal Institute of Technology (Kungliga Tekniska Högskolan), AlbaNova, SE-106 91 Stockholm, Sweden.), BA(Laboratoire Astrophysique, Interactions, Multi-échelles–Commissariat à l’Énergie Atomique (CEA)–CNRS-Université Paris Diderot, Service d’Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France.), BB(Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy.; Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy.), BC(W. W. 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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.), DJ(Laboratoire Astrophysique, Interactions, Multi-échelles–Commissariat à l’Énergie Atomique (CEA)–CNRS-Université Paris Diderot, Service d’Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France.; Laboratoire de Physique Théorique et Astroparticules, Université Montpellier 2, CNRS/IN2P3, Montpellier, France.), DK(Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA.), DL(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), DM(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), DN(CNRS/IN2P3, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.; Université de Bordeaux, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.), DO(Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy.; Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy.), DP(CNRS/IN2P3, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.; Université de Bordeaux, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.), DQ(Dipartimento di Fisica “M. 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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.), EB(Istituto di Astrofisica Spaziale e Fisica Cosmica Palermo, 90146 Palermo, Italy.), EC(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.), EE(Department of Physical Science and Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima 739-8526, Japan.), EE(Center for Research and Exploration in Space Science and Technology, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.), EF(Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari, I-70126 Bari, Italy.; Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy.), EG(W. W. 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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.), EV(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.), FF(Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy.; Dipartimento di Fisica “G. Galilei,” Università di Padova, I-35131 Padova, Italy.), FG(Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA.), FH(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), FI(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.), FJ(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.), FK(CNRS/IN2P3, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.; Université de Bordeaux, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.), FL(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.; University of Maryland, College Park, MD 20742, USA.), FM(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.), FN(Institut de Ciencies de l’Espai, Institut d’Estudis Espacials de Catalunya–Consejo Superior de Investigaciones Científicas, Campus Universitat Autonoma de Barcelona, 08193 Barcelona, Spain.), FO(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.), FP(Department of Physics, University of Washington, Seattle, WA 98195–1560, USA.), FQ(Department of Physics, Royal Institute of Technology, Kungliga Tekniska Högskolan, AlbaNova, SE-106 91 Stockholm, Sweden.), FR(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA.), FS(Laboratoire Leprince-Ringuet, École Polytechnique, CNRS/IN2P3, Palaiseau, France.), FT(Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA.), FU(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA.), FV(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA.), FW(Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden.), FX(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), FY(NYCB Real-Time Computing Inc., 18 Meudon Drive, Lattingtown, NY 11560–1025, USA.), FZ(CNRS/IN2P3, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.; Université de Bordeaux, Centre d’Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France.), GA(Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA.), GB(Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.), GC(Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari, I-70126 Bari, Italy.; Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy.), GD(Laboratoire Astrophysique, Interactions, Multi-échelles–Commissariat à l’Énergie Atomique GE(CEA –CNRS-Université Paris Diderot, Service d’Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France.), GF(Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA.), GG(Department of Chemistry and Physics, Purdue University Calumet, Hammond, IN 46323–2094, USA.), GH(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.), GI(Department of Physical Science and Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima 739-8526, Japan.), GJ(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.), GK(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.), GL(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.), GM(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.), GN(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.), GO(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA.), GP(Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy.; Dipartimento di Fisica “G. Galilei,” Università di Padova, I-35131 Padova, Italy.), GQ(Institut de Ciencies de l’Espai Institut d’Estudis Espacials de Catalunya–Consejo Superior de Investigaciones Científicas, Campus Universitat Autonoma de Barcelona, 08193 Barcelona, Spain.; Institució Catalana de Recerca i Estudis Avançats, Barcelona, Spain.), GR(Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy.; Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy.), GS(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.; Consorzio Interuniversitario per la Fisica Spaziale, I-10133 Torino, Italy.), GT(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.), GU(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.), GV(Centre d’Étude Spatiale des Rayonnements, CNRS/UPS, BP 44346, F-30128 Toulouse Cedex 4, France.), GW(Istituto Nazionale di Fisica Nucleare, Sezione di Roma “Tor Vergata” and Dipartimento di Fisica, Università di Roma “Tor Vergata,” I-00133 Roma, Italy.), GX(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.), GY(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.), GZ(Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA.), HA(Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA.), HB(Department of Physical Science and Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima 739-8526, Japan.), HC(Department of Physics, Royal Institute of Technology Kungliga Tekniska Högskolan), AlbaNova, SE-106 91 Stockholm, Sweden.; School of Pure and Applied Natural Sciences, University of Kalmar, SE-391 82 Kalmar, Sweden.), HD(Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA.)
Publication:
Science, Volume 322, Issue 5905, pp. 1218- (2008).
Publication Date:
11/2008
Category:
ASTRONOMY
Origin:
SCIENCE
DOI:
10.1126/science.1165572
Bibliographic Code:
2008Sci...322.1218A

Abstract

Energetic young pulsars and expanding blast waves [supernova remnants (SNRs)] are the most visible remains after massive stars, ending their lives, explode in core-collapse supernovae. The Fermi Gamma-Ray Space Telescope has unveiled a radio quiet pulsar located near the center of the compact synchrotron nebula inside the supernova remnant CTA 1. The pulsar, discovered through its gamma-ray pulsations, has a period of 316.86 milliseconds and a period derivative of 3.614 × 10‑13 seconds per second. Its characteristic age of 104 years is comparable to that estimated for the SNR. We speculate that most unidentified Galactic gamma-ray sources associated with star-forming regions and SNRs are such young pulsars.
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