Very high energy gamma-ray observation of the peculiar transient event Swift J1644+57 with the MAGIC telescopes and AGILE

被引：7

作者：

Aleksic, J. ^{[1
]}

Antonelli, L. A. ^{[2
]}

Antoranz, P. ^{[3
,4
]}

Asensio, M. ^{[5
]}

Backes, M. ^{[6
]}

de Almeida, U. Barres ^{[7
]}

Barrio, J. A. ^{[5
]}

Becerra Gonzalez, J. ^{[8
]}

Bednarek, W. ^{[9
]}

Berger, K. ^{[8
,10
]}

Bernardini, E. ^{[11
]}

Biland, A. ^{[12
]}

Blanch, O. ^{[1
]}

Bock, R. K. ^{[7
]}

Boller, A. ^{[12
]}

Bonnefoy, S. ^{[5
]}

Bonnoli, G. ^{[2
]}

Tridon, D. Borla ^{[7
]}

Bretz, T. ^{[13
]}

Carmona, E. ^{[14
]}

Carosi, A. ^{[2
]}

Carreto Fidalgo, D. ^{[5
,13
]}

Colin, P. ^{[7
]}

Colombo, E. ^{[8
]}

Contreras, J. L. ^{[5
]}

Cortina, J. ^{[1
]}

Cossio, L. ^{[15
,16
]}

Covino, S. ^{[2
]}

Da Vela, P. ^{[3
,4
]}

Dazzi, F. ^{[15
,16
]}

De Angelis, A. ^{[15
,16
]}

De Caneva, G. ^{[11
]}

De Lotto, B. ^{[15
,16
]}

Delgado Mendez, C. ^{[14
]}

Doert, M. ^{[6
]}

Dominguez, A. ^{[17
]}

Prester, D. Dominis ^{[18
,19
]}

Dorner, D. ^{[13
]}

Doro, M. ^{[20
,21
]}

Eisenacher, D. ^{[13
]}

Elsaesser, D. ^{[13
]}

Farina, E. ^{[22
]}

Ferenc, D. ^{[18
,19
]}

Fonseca, M. V. ^{[5
]}

Font, L. ^{[20
,21
]}

Fruck, C. ^{[7
]}

Garcia Lopez, R. J. ^{[8
,10
]}

Garczarczyk, M. ^{[8
]}

Garrido Terrats, D. ^{[20
,21
]}

Gaug, M. ^{[20
,21
]}

机构：

[1] IFAE, Bellaterra 08193, Spain

[2] INAF Natl Inst Astrophys, I-00136 Rome, Italy

[3] Univ Siena, I-53100 Siena, Italy

[4] INFN Pisa, I-53100 Siena, Italy

[5] Univ Complutense, E-28040 Madrid, Spain

[6] Tech Univ Dortmund, D-44221 Dortmund, Germany

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

[8] Inst Astrofis Canarias, Tenerife 38200, Spain

[9] Univ Lodz, PL-90236 Lodz, Poland

[10] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Spain

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

[12] ETH, CH-8093 Zurich, Switzerland

[13] Univ Wurzburg, D-97074 Wurzburg, Germany

[14] Ctr Invest Energet Medioambientales & Tecnol, Madrid 28040, Spain

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

[16] INFN Trieste, I-33100 Udine, Italy

[17] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[18] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAG Consortium, Zagreb 10000, Croatia

[19] Univ Split, Zagreb 10000, Croatia

[20] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain

[21] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain

[22] Univ Insubria, I-22100 Como, Italy

[23] CSIC, IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain

[24] Univ Turku, Tuorla Observ, Piikkio 21500, Finland

[25] Kyoto Univ, Div Phys & Astron, Japanese MAG Consortium, Kyoto 6068501, Japan

[26] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria

[27] Univ Barcelona, IEEC, ICC, E-08028 Barcelona, Spain

[28] Univ Padua, I-35131 Padua, Italy

[29] Ist Nazl Fis Nucl, I-35131 Padua, Italy

[30] INAF, Osservatorio Astron, I-34143 Trieste, Italy

[31] Ist Nazl Fis Nucl, I-34143 Trieste, Italy

[32] Univ Pisa, I-56126 Pisa, Italy

[33] Ist Nazl Fis Nucl, I-56126 Pisa, Italy

[34] ICREA, Barcelona 08010, Spain

[35] UAM, CSIC, Inst Fis Teor, Madrid 28049, Spain

[36] Univ Trieste, I-34127 Trieste, Italy

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

[38] ASI, Sci Data Ctr, I-00044 Frascati, Italy

[39] INAF Oar, I-00040 Monte Porzio Catone, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2013年 / 552卷

基金：

芬兰科学院;

关键词：

radiation mechanisms: non-thermal; galaxies: active; gamma rays: general; TIDAL DISRUPTION; BLACK-HOLES; BLAZARS; NEARBY;

D O I：

10.1051/0004-6361/201321197

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. On March 28, 2011, the BAT instrument on board the Swift satellite detected a new transient event that in the very beginning was classified as a gamma ray burst (GRB). However, the unusual X-ray flaring activity observed from a few hours up to days after the onset of the event made a different nature seem to be more likely. The long-lasting activity in the X-ray band, followed by a delayed brightening of the source in infrared and radio activity, suggested that it is better interpreted as a tidal disruption event that triggered a dormant black hole in the nucleus of the host galaxy and generated an outflowing jet of relativistic matter. Aims. Detecting a very high energy emission component from such a peculiar object would be enable us to constrain the dynamic of the emission processes and the jet model by providing information on the Doppler factor of the relativistic ejecta. Methods. The MAGIC telescopes observed the peculiar source Swift J1644+57 during the flaring phase, searching for gamma-ray emission at very-high energy (VHE, E > 100 GeV), starting observations nearly 2.5 days after the trigger time. MAGIC collected a total of 28 h of data during 12 nights. The source was observed in wobble mode during dark time at a mean zenith angle of 35 degrees. Data were reduced using a new image-cleaning algorithm, the so-called sum-cleaning, which guarantees a better noise suppression and a lower energy threshold than the standard analysis procedure. Results. No clear evidence for emission above the energy threshold of 100 GeV was found. MAGIC observations permit one to constrain the emission from the source down to 100 GeV, which favors models that explain the observed lower energy variable emission. Data analysis of simultaneous observations from AGILE, Fermi and VERITAS also provide negative detection, which additionally constrain the self-Compton emission component.

引用

页数：6

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