Multi-wavelength characterization of the blazar S5 0716+714 during an unprecedented outburst phase

被引：35

作者：

Ahnen, M. L. ^{[1
]}

Ansoldi, S. ^{[2
,28
,29
,30
,31
]}

Antonelli, L. A. ^{[3
]}

Arcaro, C. ^{[4
,39
]}

Baack, D. ^{[5
]}

Babic, A. ^{[6
,7
,8
,9
,10
]}

Banerjee, B. ^{[11
]}

Bangale, P. ^{[12
]}

Barres de Almeida, U. ^{[12
,13
]}

Barrio, J. A. ^{[14
]}

Becerra Gonzalez, J. ^{[15
,16
]}

Bednarek, W. ^{[17
]}

Bernardini, E. ^{[4
,18
,35
,39
]}

Berse, R. Ch ^{[5
]}

Berti, A. ^{[2
,36
]}

Bhattacharyya, W. ^{[18
]}

Biland, A. ^{[1
]}

Blanch, O. ^{[19
]}

Bonnoli, G. ^{[20
,21
]}

Carosi, R. ^{[20
,21
]}

Carosi, A. ^{[3
]}

Ceribella, G. ^{[12
]}

Chatterjee, A. ^{[11
]}

Colak, S. M. ^{[19
]}

Colin, P. ^{[12
]}

Colombo, E. ^{[15
,16
]}

Contreras, J. L. ^{[14
]}

Cortina, J. ^{[19
]}

Covino, S. ^{[3
]}

Cumani, P. ^{[19
]}

Da Vela, P. ^{[20
,21
]}

Dazzi, F. ^{[3
]}

De Angelis, A. ^{[4
,39
]}

De Lotto, B. ^{[2
]}

Delfino, M. ^{[19
,37
]}

Delgado, J. ^{[19
]}

Di Pierro, F. ^{[4
,39
]}

Dominguez, A. ^{[14
]}

Prester, D. Dominis ^{[6
,7
,8
,9
,10
]}

Dorner, D. ^{[22
]}

Doro, M. ^{[4
,39
]}

Einecke, S. ^{[5
]}

Elsaesser, D. ^{[5
]}

Ramazani, V. Fallah ^{[23
,24
,25
]}

Fernandez-Barral, A. ^{[4
,19
,39
]}

Fidalgo, D. ^{[14
]}

Fonseca, M., V ^{[14
]}

Font, L. ^{[26
]}

Fruck, C. ^{[12
]}

Galindo, D. ^{[27
]}

机构：

[1] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland

[2] Univ Udine, INFN Trieste, I-33100 Udine, Italy

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

[4] Univ Padua, Padua, Italy

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

[6] Croatian MAG Consortium Univ Rijeka, Rijeka 51000, Croatia

[7] Univ Split FESB, Split 21000, Croatia

[8] Univ Zagreb FER, Zagreb 10000, Croatia

[9] Univ Osijek, Osijek 31000, Croatia

[10] Rudjer Boskovic Inst, Zagreb 10000, Croatia

[11] HBNI, Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India

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

[13] CBPF, URCA, BR-22290180 Rio De Janeiro, RJ, Brazil

[14] Univ Complutense, Unidad Particulas & Cosmol UPARCOS, Madrid 28040, Spain

[15] Inst Astrofis Canarias, San Cristobal la Laguna 38200, Spain

[16] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

[17] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland

[18] DESY, D-15738 Zeuthen, Germany

[19] BIST, IFAE, Bellaterra 08193, Barcelona, Spain

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

[21] INFN Pisa, I-53100 Pisa, Italy

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

[23] Univ Turku, Finnish MAG Consortium Tuorla Observ Dept Phys &, Turku 20014, Finland

[24] Univ Turku, Finnish Ctr Astron ESO FINCA, Turku 20014, Finland

[25] Univ Oulu, Astron Div, Oulu 90014, Finland

[26] Univ Autonoma Barcelona, Dept Fis CERES IEEC, Bellaterra 08193, Spain

[27] Univ Barcelona, IEEC UB, ICC, Barcelona 08028, Spain

[28] Univ Tokyo, Japanese MAGIC Consortium ICRR, Chiba 2778582, Japan

[29] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan

[30] Tokai Univ, Kawasaki, Kanagawa 2591292, Japan

[31] Univ Tokushima, Tokushima 7708502, Japan

[32] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, Sofia 1784, Bulgaria

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

[34] INFN Pisa, I-56126 Pisa, Italy

[35] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

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

[37] PIC, Bellaterra 08193, Barcelona, Spain

[38] Univ Bologna, Dept Phys & Astron, INAF Trieste, Bologna, Italy

[39] INFN, I-35131 Padua, Italy

[40] ASI Sci Data Ctr, I-06123 Perugia, Italy

[41] INFN, I-06123 Perugia, Italy

[42] CEN Bordeaux Gradignan, F-33170 Gradignan, France

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

[44] CSIC, Inst Astrofis Andalucia, Apartado 3004, Granada 18080, Spain

[45] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[46] Crimean Astrophys Observ, P-O Nauchny, Crimea, Ukraine

[47] St Petersburg State Univ, Astron Inst, St Petersburg, Russia

[48] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[49] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland

[50] Aalto Univ, Dept Elect & Nanoengn, Aalto 00076, Finland

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 619卷

基金：

芬兰科学院; 俄罗斯科学基金会; 英国科学技术设施理事会;

关键词：

BL Lacertae objects: individual: S5 0716+714; galaxies: active; galaxies: jets; gamma rays: galaxies; EXTRAGALACTIC BACKGROUND LIGHT; LACERTAE OBJECT 0716+714; ACTIVE GALACTIC NUCLEI; GAMMA-RAY ACTIVITY; BASE-LINE ARRAY; X-RAY; 3C; 279; ELECTROMAGNETIC-SPECTRUM; MILLIMETER WAVELENGTHS; OPTICAL VARIABILITY;

D O I：

10.1051/0004-6361/201832677

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The BL Lac object S5 0716+714, a highly variable blazar, underwent an impressive outburst in January 2015 (Phase A), followed by minor activity in February (Phase B). The MAGIC observations were triggered by the optical flux observed in Phase A, corresponding to the brightest ever reported state of the source in the R-band. Aims.The comprehensive dataset collected is investigated in order to shed light on the mechanism of the broadband emission. Methods. Multi-wavelength light curves have been studied together with the broadband spectral energy distributions (SEDs). The sample includes data from Effelsberg, OVRO, Metsahovi, VLBI, CARMA, IRAM, SMA, Swift-UVOT, KVA, Tuorla, Steward, RINGO3, KANATA, AZT-8+ST7, Perkins, LX-200, Swift-XRT, NuSTAR, Fermi-LAT and MAGIC. Results. The flaring state of Phase A was detected in all the energy bands, providing for the first time a multi-wavelength sample of simultaneous data from the radio band to the very-high-energy (VHE, E> 100 GeV). In the constructed SED, the Swift-XRT +NuSTAR data constrain the transition between the synchrotron and inverse Compton components very accurately, while the second peak is constrained from 0.1 GeV to 600 GeV by Fermi+MAGIC data. The broadband SED cannot be described with a one-zone synchrotron self-Compton model as it severely underestimates the optical flux in order to reproduce the X-ray to y-ray data. Instead we use a two-zone model. The electric vector position angle (EVPA) shows an unprecedented fast rotation. An estimation of the redshift of the source by combined high-energy (HE, 0.1 GeV < E < 100 GeV) and VHE data provides a value of ,z = 0.31 +/- 0.02(stats) +/- 0.05(sys), confirming the literature value. Conclusions. The data show the VHE emission originating in the entrance and exit of a superluminal knot in and out of a recollimation shock in the inner jet. A shock-shock interaction in the jet seems responsible for the observed flares and EVPA swing. This scenario is also consistent with the SED modeling.

引用

页数：18

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