THE 2010 VERY HIGH ENERGY γ-RAY FLARE AND 10 YEARS OF MULTI-WAVELENGTH OBSERVATIONS OF M 87

被引：147

作者：

Abramowski, A. ^{[1
,20
]}

Acero, F. ^{[2
]}

Aharonian, F. ^{[3
,4
,5
]}

Akhperjanian, A. G. ^{[5
,6
]}

Anton, G. ^{[7
]}

Balzer, A. ^{[7
]}

Barnacka, A. ^{[8
,9
]}

de Almeida, U. Barres ^{[10
,46
]}

Becherini, Y. ^{[11
,12
]}

Becker, J. ^{[13
]}

Behera, B. ^{[14
]}

Bernloehr, K. ^{[3
,15
]}

Birsin, E. ^{[15
]}

Biteau, J. ^{[12
]}

Bochow, A. ^{[3
]}

Boisson, C. ^{[16
]}

Bolmont, J. ^{[17
]}

Bordas, P. ^{[18
]}

Brucker, J. ^{[7
]}

Brun, F. ^{[12
]}

Brun, P. ^{[9
]}

Bulik, T. ^{[19
]}

Buesching, I. ^{[13
,20
]}

Carrigan, S. ^{[3
]}

Casanova, S. ^{[13
]}

Cerruti, M. ^{[16
]}

Chadwick, P. M. ^{[10
]}

Charbonnier, A. ^{[17
]}

Chaves, R. C. G. ^{[3
]}

Cheesebrough, A. ^{[10
]}

Clapson, A. C. ^{[3
]}

Coignet, G. ^{[21
]}

Cologna, G. ^{[14
]}

Conrad, J. ^{[22
]}

Dalton, M. ^{[15
]}

Daniel, M. K. ^{[10
]}

Davids, I. D. ^{[23
]}

Degrange, B. ^{[12
]}

Deil, C. ^{[3
]}

Dickinson, H. J. ^{[22
]}

Djannati-Atai, A. ^{[11
]}

Domainko, W. ^{[3
]}

Drury, L. O'C. ^{[4
]}

Dubus, G. ^{[24
]}

Dutson, K. ^{[25
]}

Dyks, J. ^{[8
]}

Dyrda, M. ^{[26
]}

Egberts, K. ^{[27
]}

Eger, P. ^{[7
]}

Espigat, P. ^{[11
]}

机构：

[1] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany

[2] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72, F-34095 Montpellier 5, France

[3] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

[4] Dublin Inst Adv Studies, Dublin 2, Ireland

[5] Natl Acad Sci Republ Armenia, Yerevan 0019, Armenia

[6] Yerevan Phys Inst, Yerevan 375036, Armenia

[7] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany

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

[9] CEA Saclay, DSM IRFU, F-91191 Gif Sur Yvette, France

[10] Univ Durham, Dept Phys, Durham DH1 3LE, England

[11] Univ Paris 07, CNRS, F-75205 Paris 13, France

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

[13] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophy 4, D-44780 Bochum, Germany

[14] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany

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

[16] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France

[17] Univ Paris 07, CNRS IN2P3, Univ Paris 06, LPNHE, F-75252 Paris 5, France

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

[19] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland

[20] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa

[21] Univ Savoie, CNRS IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France

[22] Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden

[23] Univ Namibia, Dept Phys, Windhoek, Namibia

[24] Univ Grenoble 1, INSU CNRS, Lab Astrophys Grenoble, F-38041 Grenoble 9, France

[25] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[26] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland

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

[28] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland

[29] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland

[30] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[31] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic

[32] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[33] IFAE, E-08193 Bellaterra, Spain

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

[35] Univ Siena, Dipartimento Fis, I-53100 Siena, Italy

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

[37] Tech Univ Dortmund, Fak Phys, D-44221 Dortmund, Germany

[38] Univ Complutense, Grp Fis Altas Energias, E-28040 Madrid, Spain

[39] Univ Padua, Dipartimento Fis, I-35131 Padua, Italy

[40] INFN, I-35131 Padua, Italy

[41] Inst Astrofis Canarias, E-38200 Tenerife, Spain

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

[43] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland

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

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

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

[47] Univ Wurzburg, Fak Phys & Astron, D-97074 Wurzburg, Germany

[48] Univ Barcelona ICC IEEC, Fac Fis, E-08028 Barcelona, Spain

[49] Univ Udine, Dipartimento Fis Sperimentale, I-33100 Udine, Italy

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

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 746卷 / 02期

基金：

新加坡国家研究基金会; 芬兰科学院; 美国国家科学基金会; 加拿大自然科学与工程研究理事会; 爱尔兰科学基金会; 英国科学技术设施理事会;

关键词：

galaxies: active; galaxies: individual (M 87); galaxies: jets; galaxies: nuclei; gamma rays: galaxies; radiation mechanisms: non-thermal; LARGE-AREA TELESCOPE; SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEUS; M87; JET; TEV EMISSION; CRAB-NEBULA; GALAXY M-87; SCALE JETS; INNER JET; HST-1;

D O I：

10.1088/0004-637X/746/2/151

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The giant radio galaxy M 87 with its proximity (16 Mpc), famous jet, and very massive black hole ((3-6) x 10(9) M-circle dot) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100 GeV) gamma-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M 87 has been established as a VHE gamma-ray emitter since 2006. The VHE gamma-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M 87 by the MAGIC and VERITAS instruments in 2010 are reported. During the campaign, a flare at VHE was detected triggering further observations at VHE (H.E.S.S.), X-rays (Chandra), and radio (43 GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE gamma-ray light curve enables one to derive a precise temporal characterization of the flare: the single, isolated flare is well described by a two-sided exponential function with significantly different flux rise and decay times of tau(rise)(d) = (1.69 +/- 0.30) days and tau(decay)(d) = (0.611 +/- 0.080) days, respectively. While the overall variability pattern of the 2010 flare appears somewhat different from that of previous VHE flares in 2005 and 2008, they share very similar timescales (similar to day), peak fluxes (Phi(>0.35 TeV) similar or equal to (1-3) x 10(-11) photons cm(-2) s(-1)), and VHE spectra. VLBA radio observations of 43 GHz of the inner jet regions indicate no enhanced flux in 2010 in contrast to observations in 2008, where an increase of the radio flux of the innermost core regions coincided with a VHE flare. On the other hand, Chandra X-ray observations taken similar to 3 days after the peak of the VHE gamma-ray emission reveal an enhanced flux from the core (flux increased by factor similar to 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M 87, spanning from radio to VHE and including data from Hubble Space Telescope, Liverpool Telescope, Very Large Array, and European VLBI Network, is used to further investigate the origin of the VHE gamma-ray emission. No unique, common MWL signature of the three VHE flares has been identified. In the outer kiloparsec jet region, in particular in HST-1, no enhanced MWL activity was detected in 2008 and 2010, disfavoring it as the origin of the VHE flares during these years. Shortly after two of the three flares (2008 and 2010), the X-ray core was observed to be at a higher flux level than its characteristic range (determined from more than 60 monitoring observations: 2002-2009). In 2005, the strong flux dominance of HST-1 could have suppressed the detection of such a feature. Published models for VHE gamma-ray emission from M 87 are reviewed in the light of the new data.

引用

页数：18

共 107 条

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共 107 条

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Abdo, A. A. ;

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