Abstract
The giant radio galaxy M87 with its proximity (16Mpc), famous jet, and very massive black hole ((3 - 6) × 109M·) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100GeV) γ-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M87 has been established as a VHE γ-ray emitter since 2006. The VHE γ-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M87 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 (43GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE γ-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 τrise d = (1.69 ± 0.30) days and τdecay 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 (day), peak fluxes (Φ>0.35 TeV ≃ (1-3) × 10-11 photonscm-2 s-1), and VHE spectra. VLBA radio observations of 43GHz 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 3 days after the peak of the VHE γ-ray emission reveal an enhanced flux from the core (flux increased by factor 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M87, 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 γ-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 γ-ray emission from M87 are reviewed in the light of the new data.
| Original language | English (US) |
|---|---|
| Article number | 151 |
| Journal | Astrophysical Journal |
| Volume | 746 |
| Issue number | 2 |
| DOIs | |
| State | Published - Feb 20 2012 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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In: Astrophysical Journal, Vol. 746, No. 2, 151, 20.02.2012.
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T1 - The 2010 very high energy γ-ray flare and 10 years of multi-wavelength observations of M 87
AU - Abramowski, A.
AU - Acero, F.
AU - Aharonian, F.
AU - Akhperjanian, A. G.
AU - Anton, G.
AU - Balzer, A.
AU - Barnacka, A.
AU - Barres De Almeida, U.
AU - Becherini, Y.
AU - Becker, J.
AU - Behera, B.
AU - Bernlöhr, K.
AU - Birsin, E.
AU - Biteau, J.
AU - Bochow, A.
AU - Boisson, C.
AU - Bolmont, J.
AU - Bordas, P.
AU - Brucker, J.
AU - Brun, F.
AU - Brun, P.
AU - Bulik, T.
AU - Büsching, I.
AU - Carrigan, S.
AU - Casanova, S.
AU - Cerruti, M.
AU - Chadwick, P. M.
AU - Charbonnier, A.
AU - Chaves, R. C.G.
AU - Cheesebrough, A.
AU - Clapson, A. C.
AU - Coignet, G.
AU - Cologna, G.
AU - Conrad, J.
AU - Dalton, M.
AU - Daniel, M. K.
AU - Davids, I. D.
AU - Degrange, B.
AU - Deil, C.
AU - Dickinson, H. J.
AU - Djannati-Ata, A.
AU - Domainko, W.
AU - Drury, L. O.
AU - Dubus, G.
AU - Dutson, K.
AU - Dyks, J.
AU - Dyrda, M.
AU - Egberts, K.
AU - Eger, P.
AU - Espigat, P.
AU - Fallon, L.
AU - Farnier, C.
AU - Fegan, S.
AU - Feinstein, F.
AU - Fernandes, M. V.
AU - Fiasson, A.
AU - Fontaine, G.
AU - Förster, A.
AU - Füling, M.
AU - Gallant, Y. A.
AU - Gast, H.
AU - Gérard, L.
AU - Gerbig, D.
AU - Giebels, B.
AU - Glicenstein, J. F.
AU - Glück, B.
AU - Goret, P.
AU - Göring, D.
AU - Häffner, S.
AU - Hague, J. D.
AU - Hampf, D.
AU - Hauser, M.
AU - Heinz, S.
AU - Heinzelmann, G.
AU - Henri, G.
AU - Hermann, G.
AU - Hinton, J. A.
AU - Hoffmann, A.
AU - Hofmann, W.
AU - Hofverberg, P.
AU - Holler, M.
AU - Horns, D.
AU - Jacholkowska, A.
AU - De Jager, O. C.
AU - Jahn, C.
AU - Jamrozy, M.
AU - Jung, I.
AU - Kastendieck, M. A.
AU - Katarzyński, K.
AU - Katz, U.
AU - Kaufmann, S.
AU - Keogh, D.
AU - Khangulyan, D.
AU - Khélifi, B.
AU - Klochkov, D.
AU - Kluźniak, W.
AU - Kneiske, T.
AU - Komin, Nu
AU - Kosack, K.
AU - Kossakowski, R.
AU - Laffon, H.
AU - Lamanna, G.
AU - Lennarz, D.
AU - Lohse, T.
AU - Lopatin, A.
AU - Lu, C. C.
AU - Marandon, V.
AU - Marcowith, A.
AU - Masbou, J.
AU - Maurin, D.
AU - Maxted, N.
AU - Mayer, M.
AU - McComb, T. J.L.
AU - Medina, M. C.
AU - Méhault, J.
AU - Moderski, R.
AU - Moulin, E.
AU - Naumann, C. L.
AU - Naumann-Godo, M.
AU - De Naurois, M.
AU - Nedbal, D.
AU - Nekrassov, D.
AU - Nguyen, N.
AU - Nicholas, B.
AU - Niemiec, J.
AU - Nolan, S. J.
AU - Ohm, S.
AU - De Õa Wilhelmi, E.
AU - Opitz, B.
AU - Ostrowski, M.
AU - Oya, I.
AU - Panter, M.
AU - Paz Arribas, M.
AU - Pedaletti, G.
AU - Pelletier, G.
AU - Petrucci, P. O.
AU - Pita, S.
AU - Pühlhofer, G.
AU - Punch, M.
AU - Quirrenbach, A.
AU - Raue, M.
AU - Rayner, S. M.
AU - Reimer, A.
AU - Reimer, O.
AU - Renaud, M.
AU - De Los Reyes, R.
AU - Rieger, F.
AU - Ripken, J.
AU - Rob, L.
AU - Rosier-Lees, S.
AU - Rowell, G.
AU - Rudak, B.
AU - Rulten, C. B.
AU - Ruppel, J.
AU - Sahakian, V.
AU - Sanchez, D. A.
AU - Santangelo, A.
AU - Schlickeiser, R.
AU - Schöck, F. M.
AU - Schulz, A.
AU - Schwanke, U.
AU - Schwarzburg, S.
AU - Schwemmer, S.
AU - Sheidaei, F.
AU - Skilton, J. L.
AU - Sol, H.
AU - Spengler, G.
AU - Stawarz,
AU - Steenkamp, R.
AU - Stegmann, C.
AU - Stinzing, F.
AU - Stycz, K.
AU - Sushch, I.
AU - Szostek, A.
AU - Tavernet, J. P.
AU - Terrier, R.
AU - Tluczykont, M.
AU - Valerius, K.
AU - Van Eldik, C.
AU - Vasileiadis, G.
AU - Venter, C.
AU - Vialle, J. P.
AU - Viana, A.
AU - Vincent, P.
AU - Völk, H. J.
AU - Volpe, F.
AU - Vorobiov, S.
AU - Vorster, M.
AU - Wagner, S. J.
AU - Ward, M.
AU - White, R.
AU - Wierzcholska, A.
AU - Zacharias, M.
AU - Zajczyk, A.
AU - Zdziarski, A. A.
AU - Zech, A.
AU - Zechlin, H. S.
AU - Aleksić, J.
AU - Antonelli, L. A.
AU - Antoranz, P.
AU - Backes, M.
AU - Barrio, J. A.
AU - Bastieri, D.
AU - Becerra Gonzlez, J.
AU - Bednarek, W.
AU - Berdyugin, A.
AU - Berger, K.
AU - Bernardini, E.
AU - Biland, A.
AU - Blanch, O.
AU - Bock, R. K.
AU - Boller, A.
AU - Bonnoli, G.
AU - Borla Tridon, D.
AU - Braun, I.
AU - Bretz, T.
AU - Cãellas, A.
AU - Carmona, E.
AU - Carosi, A.
AU - Colin, P.
AU - Colombo, E.
AU - Contreras, J. L.
AU - Cortina, J.
AU - Cossio, L.
AU - Covino, S.
AU - Dazzi, F.
AU - De Angelis, A.
AU - De Cea Del Pozo, E.
AU - De Lotto, B.
AU - Delgado Mendez, C.
AU - Diago Ortega, A.
AU - Doert, M.
AU - Domínguez, A.
AU - Dominis Prester, D.
AU - Dorner, D.
AU - Doro, M.
AU - Elsaesser, D.
AU - Ferenc, D.
AU - Fonseca, M. V.
AU - Font, L.
AU - Fruck, C.
AU - García López, R. J.
AU - Garczarczyk, M.
AU - Garrido, D.
AU - Giavitto, G.
AU - Godinović, N.
AU - Hadasch, D.
AU - Häfner, D.
AU - Herrero, A.
AU - Hildebrand, D.
AU - Höhne-Mönch, D.
AU - Hose, J.
AU - Hrupec, D.
AU - Huber, B.
AU - Jogler, T.
AU - Klepser, S.
AU - Krähenbühl, T.
AU - Krause, J.
AU - La Barbera, A.
AU - Lelas, D.
AU - Leonardo, E.
AU - Lindfors, E.
AU - Lombardi, S.
AU - López, M.
AU - Lorenz, E.
AU - Makariev, M.
AU - Maneva, G.
AU - Mankuzhiyil, N.
AU - Mannheim, K.
AU - Maraschi, L.
AU - Mariotti, M.
AU - Martínez, M.
AU - Mazin, D.
AU - Meucci, M.
AU - Miranda, J. M.
AU - Mirzoyan, R.
AU - Miyamoto, H.
AU - Moldón, J.
AU - Moralejo, A.
AU - Munar, P.
AU - Nieto, D.
AU - Nilsson, K.
AU - Orito, R.
AU - Oya, I.
AU - Paneque, D.
AU - Paoletti, R.
AU - Pardo, S.
AU - Paredes, J. M.
AU - Partini, S.
AU - Pasanen, M.
AU - Pauss, F.
AU - Perez-Torres, M. A.
AU - Persic, M.
AU - Peruzzo, L.
AU - Pilia, M.
AU - Pochon, J.
AU - Prada, F.
AU - Prada Moroni, P. G.
AU - Prandini, E.
AU - Puljak, I.
AU - Reichardt, I.
AU - Reinthal, R.
AU - Rhode, W.
AU - Ribó, M.
AU - Rico, J.
AU - Rügamer, S.
AU - Saggion, A.
AU - Saito, K.
AU - Saito, T. Y.
AU - Salvati, M.
AU - Satalecka, K.
AU - Scalzotto, V.
AU - Scapin, V.
AU - Schultz, C.
AU - Schweizer, T.
AU - Shayduk, M.
AU - Shore, S. N.
AU - Sillanpää, A.
AU - Sitarek, J.
AU - Sobczynska, D.
AU - Spanier, F.
AU - Spiro, S.
AU - Stamerra, A.
AU - Steinke, B.
AU - Storz, J.
AU - Strah, N.
AU - Surić, T.
AU - Takalo, L.
AU - Takami, H.
AU - Tavecchio, F.
AU - Temnikov, P.
AU - Terzić, T.
AU - Tescaro, D.
AU - Teshima, M.
AU - Thom, M.
AU - Tibolla, O.
AU - Torres, D. F.
AU - Treves, A.
AU - Vankov, H.
AU - Vogler, P.
AU - Wagner, R. M.
AU - Weitzel, Q.
AU - Zabalza, V.
AU - Zandanel, F.
AU - Zanin, R.
AU - Arlen, T.
AU - Aune, T.
AU - Beilicke, M.
AU - Benbow, W.
AU - Bouvier, A.
AU - Bradbury, S. M.
AU - Buckley, J. H.
AU - Bugaev, V.
AU - Byrum, K.
AU - Cannon, A.
AU - Cesarini, A.
AU - Ciupik, L.
AU - Connolly, M. P.
AU - Cui, W.
AU - Dickherber, R.
AU - Duke, C.
AU - Errando, M.
AU - Falcone, A.
AU - Finley, J. P.
AU - Finnegan, G.
AU - Fortson, L.
AU - Furniss, A.
AU - Galante, N.
AU - Gall, D.
AU - Godambe, S.
AU - Griffin, S.
AU - Grube, J.
AU - Gyuk, G.
AU - Hanna, D.
AU - Holder, J.
AU - Huan, H.
AU - Hui, C. M.
AU - Kaaret, P.
AU - Karlsson, N.
AU - Kertzman, M.
AU - Khassen, Y.
AU - Kieda, D.
AU - Krawczynski, H.
AU - Krennrich, F.
AU - Lang, M. J.
AU - Lebohec, S.
AU - Maier, G.
AU - McArthur, S.
AU - McCann, A.
AU - Moriarty, P.
AU - Mukherjee, R.
AU - Nũez, P. D.
AU - Ong, R. A.
AU - Orr, M.
AU - Otte, A. N.
AU - Park, N.
AU - Perkins, J. S.
AU - Pichel, A.
AU - Pohl, M.
AU - Prokoph, H.
AU - Ragan, K.
AU - Reyes, L. C.
AU - Reynolds, P. T.
AU - Roache, E.
AU - Rose, H. J.
AU - Ruppel, J.
AU - Schroedter, M.
AU - Sembroski, G. H.
AU - Şentürk, G. D.
AU - Telezhinsky, I.
AU - Teić, G.
AU - Theiling, M.
AU - Thibadeau, S.
AU - Varlotta, A.
AU - Vassiliev, V. V.
AU - Vivier, M.
AU - Wakely, S. P.
AU - Weekes, T. C.
AU - Williams, D. A.
AU - Zitzer, B.
AU - Barres De Almeida, U.
AU - Cara, M.
AU - Casadio, C.
AU - Cheung, C. C.
AU - McConville, W.
AU - Davies, F.
AU - Doi, A.
AU - Giovannini, G.
AU - Giroletti, M.
AU - Hada, K.
AU - Hardee, P.
AU - Harris, D. E.
AU - Junor, W.
AU - Kino, M.
AU - Lee, N. P.
AU - Ly, C.
AU - Madrid, J.
AU - Massaro, F.
AU - Mundell, C. G.
AU - Nagai, H.
AU - Perlman, E. S.
AU - Steele, I. A.
AU - Walker, R. C.
AU - Wood, D. L.
PY - 2012/2/20
Y1 - 2012/2/20
N2 - The giant radio galaxy M87 with its proximity (16Mpc), famous jet, and very massive black hole ((3 - 6) × 109M·) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100GeV) γ-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M87 has been established as a VHE γ-ray emitter since 2006. The VHE γ-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M87 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 (43GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE γ-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 τrise d = (1.69 ± 0.30) days and τdecay 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 (day), peak fluxes (Φ>0.35 TeV ≃ (1-3) × 10-11 photonscm-2 s-1), and VHE spectra. VLBA radio observations of 43GHz 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 3 days after the peak of the VHE γ-ray emission reveal an enhanced flux from the core (flux increased by factor 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M87, 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 γ-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 γ-ray emission from M87 are reviewed in the light of the new data.
AB - The giant radio galaxy M87 with its proximity (16Mpc), famous jet, and very massive black hole ((3 - 6) × 109M·) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100GeV) γ-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M87 has been established as a VHE γ-ray emitter since 2006. The VHE γ-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M87 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 (43GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE γ-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 τrise d = (1.69 ± 0.30) days and τdecay 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 (day), peak fluxes (Φ>0.35 TeV ≃ (1-3) × 10-11 photonscm-2 s-1), and VHE spectra. VLBA radio observations of 43GHz 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 3 days after the peak of the VHE γ-ray emission reveal an enhanced flux from the core (flux increased by factor 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M87, 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 γ-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 γ-ray emission from M87 are reviewed in the light of the new data.
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U2 - 10.1088/0004-637X/746/2/151
DO - 10.1088/0004-637X/746/2/151
M3 - Article
AN - SCOPUS:84856903650
SN - 0004-637X
VL - 746
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 151
ER -