DISCOVERY OF HIGH-ENERGY GAMMA-RAY EMISSION FROM THE BINARY SYSTEM PSR B1259-63/LS 2883 AROUND PERIASTRON WITH FERMI

被引：89

作者：

Abdo, A. A. ^{[28
,40
]}

Ackermann, M. ^{[1
,2
]}

Ajello, M. ^{[1
,2
]}

Allafort, A. ^{[1
,2
]}

Ballet, J. ^{[3
]}

Barbiellini, G. ^{[4
,5
]}

Bastieri, D. ^{[6
,7
]}

Bechtol, K. ^{[1
,2
]}

Bellazzini, R. ^{[8
]}

Berenji, B. ^{[1
,2
]}

Blandford, R. D. ^{[1
,2
]}

Bonamente, E. ^{[9
,10
]}

Borgland, A. W. ^{[1
,2
]}

Bregeon, J. ^{[8
]}

Brigida, M. ^{[11
,12
]}

Bruel, P. ^{[13
]}

Buehler, R. ^{[1
,2
]}

Buson, S. ^{[6
,7
]}

Caliandro, G. A. ^{[14
]}

Cameron, R. A. ^{[1
,2
]}

Camilo, F. ^{[15
]}

Caraveo, P. A. ^{[16
]}

Cecchi, C. ^{[9
,10
]}

Charles, E. ^{[1
,2
]}

Chaty, S. ^{[3
]}

Chekhtman, A. ^{[17
]}

Chernyakova, M. ^{[18
]}

Cheung, C. C. ^{[19
]}

Chiang, J. ^{[1
,2
]}

Ciprini, S. ^{[10
]}

Claus, R. ^{[1
,2
]}

Cohen-Tanugi, J. ^{[20
]}

Cominsky, L. R. ^{[21
]}

Corbel, S. ^{[3
,22
]}

Cutini, S. ^{[23
]}

D'Ammando, F. ^{[24
,25
]}

de Angelis, A. ^{[26
,27
]}

den Hartog, P. R. ^{[1
,2
]}

de Palma, F. ^{[11
,12
]}

Dermer, C. D. ^{[28
]}

Digel, S. W. ^{[1
,2
]}

do Couto e Silva, E. ^{[1
,2
]}

Dormody, M. ^{[29
,30
]}

Drell, P. S. ^{[1
,2
]}

Drlica-Wagner, A. ^{[1
,2
]}

Dubois, R. ^{[1
,2
]}

Dubus, G. ^{[31
]}

Dumora, D. ^{[32
]}

Enoto, T. ^{[1
,2
]}

Espinoza, C. M. ^{[33
]}

机构：

[1] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA

[2] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[3] Univ Paris Diderot, CEA Saclay, Lab AIM, CEA,IRFU,CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France

[4] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[5] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[6] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[7] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy

[8] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[9] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[10] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[11] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[12] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[13] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[14] CSIC, IEEC, Inst Ciencias Espai, Barcelona 08193, Spain

[15] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[16] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy

[17] Artep Inc, Ellicott City, MD 21042 USA

[18] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland

[19] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA

[20] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France

[21] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA

[22] Inst Univ France, F-75005 Paris, France

[23] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy

[24] IASF Palermo, I-90146 Palermo, Italy

[25] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy

[26] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[27] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[28] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA

[29] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[30] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[31] Univ Grenoble 1, Inst Planetol & Astrophys Grenoble, CNRS, INSU,UMR 5274, F-38041 Grenoble, France

[32] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France

[33] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England

[34] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[35] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[36] INAF Ist Radioastron, I-40129 Bologna, Italy

[37] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany

[38] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37240 USA

[39] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA

[40] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA

[41] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland

[42] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[43] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[44] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia

[45] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

[46] IRAP, CNRS, F-31028 Toulouse 4, France

[47] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France

[48] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[49] CRESST, Greenbelt, MD 20771 USA

[50] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 736卷 / 01期

基金：

瑞典研究理事会;

关键词：

binaries: eclipsing; gamma rays: stars; pulsars: individual (PSR B1259-63); X-rays: binaries; PULSAR; RADIO; TELESCOPE; PASSAGE; PSR-B1259-63/SS2883; PSR-1259-63; RADIATION; CATALOG; WIND;

D O I：

10.1088/2041-8205/736/1/L11

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the discovery of >= 100 MeV gamma-rays from the binary system PSR B1259-63/LS 2883 using the Large Area Telescope (LAT) on board Fermi. The system comprises a radio pulsar in orbit around a Be star. We report on LAT observations from near apastron to similar to 128 days after the time of periastron, t(p), on 2010 December 15. No gamma-ray emission was detected from this source when it was far from periastron. Faint gamma-ray emission appeared as the pulsar approached periastron. At similar to t(p) + 30 days, the >= 100 MeV gamma-ray flux increased over a period of a few days to a peak flux 20-30 times that seen during the pre-periastron period, but with a softer spectrum. For the following month, it was seen to be variable on daily timescales, but remained at similar to(1-4) x 10(-6) cm(-2) s(-1) before starting to fade at similar to t(p) + 57 days. The total gamma-ray luminosity observed during this period is comparable to the spin-down power of the pulsar. Simultaneous radio and X-ray observations of the source showed no corresponding dramatic changes in radio and X-ray flux between the pre-periastron and post-periastron flares. We discuss possible explanations for the observed gamma-ray-only flaring of the source.

引用

页数：6

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