MINUTE-TIMESCALE > 100 MeV γ-RAY VARIABILITY DURING THE GIANT OUTBURST OF QUASAR 3C 279 OBSERVED BY FERMI-LAT IN 2015 JUNE

被引：178

作者：

Ackermann, M. ^{[1
]}

Anantua, R. ^{[2
,3
]}

Asano, K. ^{[4
]}

Baldini, L. ^{[2
,3
,5
,6
]}

Barbiellini, G. ^{[7
,8
]}

Bastieri, D. ^{[9
,10
]}

Gonzalez, J. Becerra ^{[11
,12
,13
]}

Bellazzini, R. ^{[6
]}

Bissaldi, E. ^{[14
]}

Blandford, R. D. ^{[2
,3
]}

Bloom, E. D. ^{[2
,3
]}

Bonino, R. ^{[15
,16
]}

Bottacini, E. ^{[2
,3
]}

Bruel, P. ^{[17
]}

Buehler, R. ^{[1
]}

Caliandro, G. A. ^{[2
,3
,18
]}

Cameron, R. A. ^{[2
,3
]}

Caragiulo, M. ^{[14
,19
,20
]}

Caraveo, P. A. ^{[21
]}

Cavazzuti, E. ^{[22
]}

Cecchi, C. ^{[23
,24
]}

Cheung, C. C. ^{[25
]}

Chiang, J. ^{[2
,3
]}

Chiaro, G. ^{[10
]}

Ciprini, S. ^{[23
]}

Cohen-Tanugi, J. ^{[26
]}

Costanza, F. ^{[14
]}

Cutini, S. ^{[22
,23
]}

D'Ammando, F. ^{[27
,28
]}

De Palma, F. ^{[14
]}

Desiante, R. ^{[15
,29
]}

Digel, S. W. ^{[2
,3
]}

Di Lalla, N. ^{[6
]}

Di Mauro, M. ^{[2
,3
]}

Di Venere, L. ^{[14
,19
,20
]}

Drell, P. S. ^{[2
,3
]}

Favuzzi, C. ^{[14
,19
,20
]}

Fegan, S. J. ^{[17
]}

Ferrara, E. C. ^{[11
]}

Fukazawa, Y. ^{[30
]}

Funk, S. ^{[31
]}

Fusco, P. ^{[19
,20
]}

Gargano, F. ^{[14
]}

Gasparrini, D. ^{[23
]}

Giglietto, N. ^{[14
,19
,20
]}

Giordano, F. ^{[14
,19
,20
]}

Giroletti, M. ^{[27
]}

Grenier, I. A. ^{[32
]}

Guillemot, L. ^{[33
,34
]}

Guiriec, S.

机构：

[1] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

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

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

[4] Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan

[5] Univ Pisa, I-56127 Pisa, Italy

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

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

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

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

[10] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

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

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

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

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

[15] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[16] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy

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

[18] CIFS, I-10133 Turin, Italy

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

[20] Politecn Bari, I-70126 Bari, Italy

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

[22] ASI, Sci Data Ctr, I-00133 Rome, Italy

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

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

[25] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA

[26] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France

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

[28] Univ Telemat Pegaso, Piazza Trieste Trento 48, I-80132 Naples, Italy

[29] Univ Udine, I-33100 Udine, Italy

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

[31] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

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

[33] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France

[34] INSU, CNRS, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France

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

[36] AlbaNova, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden

[37] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

[38] CSIC, Inst Space Sci IEEC, Campus UAB, E-08193 Barcelona, Spain

[39] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, BP120, F-33175 Gradignan, France

[40] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

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

[42] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland

[43] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[44] Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa

[45] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[46] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

[47] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA

[48] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA

[49] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland

[50] ICREA, Barcelona, Spain

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2016年 / 824卷 / 02期

基金：

瑞典研究理事会;

关键词：

galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (3C 279); radiation mechanisms: non-thermal; LARGE-AREA TELESCOPE; MULTIWAVELENGTH OBSERVATIONS; RAPID VARIABILITY; RELATIVISTIC JET; CRAB-NEBULA; EMISSION; BLAZARS; RADIATION; FLARES; LOCATION;

D O I：

10.3847/2041-8205/824/2/L20

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

On 2015 June 16, Fermi- LAT observed a giant outburst from the flat spectrum radio quasar 3C 279 with a peak >100 MeV flux of similar to 3.6 x 10(-5) photons cm(-2) s(-1), averaged over orbital period intervals. It is historically the highest gamma-ray flux observed from the source, including past EGRET observations, with the gamma-ray isotropic luminosity reaching similar to 10(49) erg s(-1). During the outburst, the Fermi spacecraft, which has an orbital period of 95.4 minutes, was operated in a special pointing mode to optimize the exposure for 3C 279. For the first time, significant flux variability at sub-orbital timescales was found in blazar observations by Fermi- LAT. The source flux variability was resolved down to 2-minute binned timescales, with flux doubling times of less than 5 minutes. The observed minute-scale variability suggests a very compact emission region at hundreds of Schwarzschild radii from the central engine in conical jet models. A minimum bulk jet Lorentz factor (Gamma) of 35 is necessary to avoid both internal gamma-ray absorption and super-Eddington jet power. In the standard external radiation Comptonization scenario, G should be at least 50 to avoid overproducing the synchrotron self-Compton component. However, this predicts extremely low magnetization (similar to 5 x 10(-4)). Equipartition requires Gamma as high as 120, unless the emitting region is a small fraction of the dissipation region. Alternatively, we consider. rays originating as synchrotron radiation of gamma e similar to 1.6 x 10(6) electrons, in a magnetic field B similar to 1.3 kG, accelerated by strong electric fields E similar to B in the process of magnetoluminescence. At such short distance scales, one cannot immediately exclude the production of gamma-rays in hadronic processes.

引用

页数：8

共 38 条

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← 1 2 3 4 →

共 38 条

[1] Gamma-Ray Flares from the Crab Nebula
Abdo, A. A.
Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Brandt, T. J.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Cannon, A.
Caraveo, P. A.
Casandjian, J. M.
Celik, O.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Costamante, L.
Cutini, S.
D'Ammando, F.
Dermer, C. D.
de Angelis, A.
de Luca, A.
de Palma, F.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Dubois, R.
Dumora, D.
Favuzzi, C.
[J]. SCIENCE, 2011, 331 (6018) : 739 - 742
[2] DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA
Acero, F.
Ackermann, M.
Ajello, M.
Albert, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Bloom, E. D.
Bonino, R.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Funk, S.
Fusco, P.
Gargano, F.
[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 2016, 223 (02)
[3] FERMI LARGE AREA TELESCOPE THIRD SOURCE CATALOG
Acero, F.
Ackermann, M.
Ajello, M.
Albert, A.
Atwood, W. B.
Axelsson, M.
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MINUTE-TIMESCALE &gt; 100 MeV γ-RAY VARIABILITY DURING THE GIANT OUTBURST OF QUASAR 3C 279 OBSERVED BY FERMI-LAT IN 2015 JUNE

MINUTE-TIMESCALE > 100 MeV γ-RAY VARIABILITY DURING THE GIANT OUTBURST OF QUASAR 3C 279 OBSERVED BY FERMI-LAT IN 2015 JUNE