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Fermi LARGE AREA TELESCOPE OBSERVATIONS OF BLAZAR 3C 279 OCCULTATIONS BY THE SUN.
Barbiellini, G; Bastieri, D; Bechtol, K; Bellazzini, R; Blandford, R D; Borgland, A W; Bregeon, J; Bruel, P; Buehler, R; Buson, S; Caliandro, G A; Cameron, R A; Caraveo, P A; Cavazzuti, E; Cecchi, C; Chaves, R C G; Chekhtman, A; Cheung, C C; Chiang, J; Ciprini, S; Claus, R; Cohen-Tanugi, J; D'Ammando, F; de Angelis, A; Dermer, C D; Digel, S W; do Couto E Silva, E; Drell, P S; Drlica-Wagner, A; Favuzzi, C; Focke, W B; Franckowiak, A; Fukazawa, Y; Fusco, P; Gargano, F; Gasparrini, D; Germani, S; Giglietto, N; Giommi, P; Giordano, F; Giroletti, M; Glanzman, T; Godfrey, G; Grenier, I A; Grove, J E; Guiriec, S; Hadasch, D; Hayashida, M; Hays, E; Hughes, R E.
Afiliação
  • Barbiellini G; Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy.
  • Bastieri D; Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy.
  • Bechtol K; Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy.
  • Bellazzini R; Dipartimento di Fisica e Astronomia "G. Galilei," Università di Padova, I-35131 Padova, Italy.
  • Blandford RD; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Borgland AW; Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.
  • Bregeon J; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Bruel P; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Buehler R; Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy.
  • Buson S; Laboratoire Leprince-Ringuet, École polytechnique, CNRS/IN2P3, Palaiseau, France.
  • Caliandro GA; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Cameron RA; Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy.
  • Caraveo PA; Dipartimento di Fisica e Astronomia "G. Galilei," Università di Padova, I-35131 Padova, Italy.
  • Cavazzuti E; Institut de Ciències de l'Espai (IEEE-CSIC), Campus UAB, E-08193 Barcelona, Spain.
  • Cecchi C; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Chaves RCG; INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica, I-20133 Milano, Italy.
  • Chekhtman A; Agenzia Spaziale Italiana (ASI) Science Data Center, I-00044 Frascati (Roma), Italy.
  • Cheung CC; Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy.
  • Chiang J; Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy.
  • Ciprini S; Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d'Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France.
  • Claus R; Center for Earth Observing and Space Research, College of Science, George Mason University, Fairfax, VA 22030, USA.
  • Cohen-Tanugi J; Resident at Naval Research Laboratory, Washington, DC 20375, USA.
  • D'Ammando F; National Research Council Research Associate, National Academy of Sciences, Washington, DC 20001, USA.
  • de Angelis A; Current address: Max-Planck-Institut für Astrophysik, D-85741 München, Germany.
  • Dermer CD; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Digel SW; Agenzia Spaziale Italiana (ASI) Science Data Center, I-00044 Frascati (Roma), Italy.
  • do Couto E Silva E; Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy.
  • Drell PS; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Drlica-Wagner A; Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, Montpellier, France.
  • Favuzzi C; Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy.
  • Focke WB; IASF Palermo, 90146 Palermo, Italy.
  • Franckowiak A; INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica, I-00133 Roma, Italy.
  • Fukazawa Y; Dipartimento di Fisica, Università di Udine and Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Gruppo Collegato di Udine, I-33100 Udine, Italy.
  • Fusco P; Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA.
  • Gargano F; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Gasparrini D; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Germani S; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Giglietto N; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Giommi P; Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy.
  • Giordano F; Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy.
  • Giroletti M; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Glanzman T; W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA.
  • Godfrey G; Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan.
  • Grenier IA; Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy.
  • Grove JE; Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy.
  • Guiriec S; Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy.
  • Hadasch D; Agenzia Spaziale Italiana (ASI) Science Data Center, I-00044 Frascati (Roma), Italy.
  • Hayashida M; Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy.
  • Hays E; Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy.
  • Hughes RE; Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy.
Astrophys J ; 784(2)2014 Apr 01.
Article em En | MEDLINE | ID: mdl-34646038
ABSTRACT
Observations of occultations of bright γ-ray sources by the Sun may reveal predicted pair halos around blazars and/or new physics, such as, e.g., hypothetical light dark matter particles-axions. We use Fermi Gamma-Ray Space Telescope (Fermi) data to analyze four occultations of blazar 3C 279 by the Sun on October 8 each year from 2008 to 2011. A combined analysis of the observations of these occultations allows a point-like source at the position of 3C 279 to be detected with significance of ≈3σ, but does not reveal any significant excess over the flux expected from the quiescent Sun. The likelihood ratio test rules out complete transparency of the Sun to the blazar γ-ray emission at a 3σ confidence level.
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Texto completo: 1 Base de dados: MEDLINE Idioma: En Revista: Astrophys J Ano de publicação: 2014 Tipo de documento: Article País de afiliação: Itália
Texto completo
Imprimir
XML
PubMed Links
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Texto completo: 1 Base de dados: MEDLINE Idioma: En Revista: Astrophys J Ano de publicação: 2014 Tipo de documento: Article País de afiliação: Itália