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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.
THE 2010 VERY HIGH ENERGY gamma-RAY FLARE AND 10 YEARS OF MULTI-WAVELENGTH OBSERVATIONS OF M 87
Abramowski A.;Acero F.;Aharonian F.;Akhperjanian A. G.;Anton G.;Balzer A.;Barnacka A.;de Almeida U. Barres;Becherini Y.;Becker J.;Behera B.;Bernloehr K.;Birsin E.;Biteau J.;Bochow A.;Boisson C.;Bolmont J.;Bordas P.;Brucker J.;Brun F.;Brun P.;Bulik T.;Buesching I.;Carrigan S.;Casanova S.;Cerruti M.;Chadwick P. M.;Charbonnier A.;Chaves R. C. G.;Cheesebrough A.;Clapson A. C.;Coignet G.;Cologna G.;Conrad J.;Dalton M.;Daniel M. K.;Davids I. D.;Degrange B.;Deil C.;Dickinson H. J.;Djannati Atai A.;Domainko W.;Drury L. O.'.C.;Dubus G.;Dutson K.;Dyks J.;Dyrda M.;Egberts K.;Eger P.;Espigat P.;Fallon L.;Farnier C.;Fegan S.;Feinstein F.;Fernandes M. V.;Fiasson A.;Fontaine G.;Foerster A.;Fuessling M.;Gallant Y. A.;Gast H.;Gerard L.;Gerbig D.;Giebels B.;Glicenstein J. F.;Glueck B.;Goret P.;Goering D.;Haeffner S.;Hague J. D.;Hampf D.;Hauser M.;Heinz S.;Heinzelmann G.;Henri G.;Hermann G.;Hinton J. A.;Hoffmann A.;Hofmann W.;Hofverberg P.;Holler M.;Horns D.;Jacholkowska A.;de Jager O. C.;Jahn C.;Jamrozy M.;Jung I.;Kastendieck M. A.;Katarzynski K.;Katz U.;Kaufmann S.;Keogh D.;Khangulyan D.;Khelifi B.;Klochkov D.;Kluzniak W.;Kneiske T.;Komin N.u.;Kosack K.;Kossakowski R.;Laffon H.;Lamanna G.;Lennarz D.;Lohse T.;Lopatin A.;Lu C. C.;Marandon V.;Marcowith A.;Masbou J.;Maurin D.;Maxted N.;Mayer M.;McComb T. J. L.;Medina M. C.;Mehault J.;Moderski R.;Moulin E.;Naumann C. L.;Naumann Godo M.;de Naurois M.;Nedbal D.;Nekrassov D.;Nguyen N.;Nicholas B.;Niemiec J.;Nolan S. J.;Ohm S.;Wilhelmi E. de Ona;Opitz B.;Ostrowski M.;Oya I.;Panter M.;Arribas M. Paz;Pedaletti G.;Pelletier G.;Petrucci P. O.;Pita S.;Puehlhofer G.;Punch M.;Quirrenbach A.;Raue M.;Rayner S. M.;Reimer A.;Reimer O.;Renaud M.;de los Reyes R.;Rieger F.;Ripken J.;Rob L.;Rosier Lees S.;Rowell G.;Rudak B.;Rulten C. B.;Ruppel J.;Sahakian V.;Sanchez D. A.;Santangelo A.;Schlickeiser R.;Schoeck F. M.;Schulz A.;Schwanke U.;Schwarzburg S.;Schwemmer S.;Sheidaei F.;Skilton J. L.;Sol H.;Spengler G.;Stawarz L.;Steenkamp R.;Stegmann C.;Stinzing F.;Stycz K.;Sushch I.;Szostek A.;Tavernet J. P.;Terrier R.;Tluczykont M.;Valerius K.;van Eldik C.;Vasileiadis G.;Venter C.;Vialle J. P.;Viana A.;Vincent P.;Voelk H. J.;Volpe F.;Vorobiov S.;Vorster M.;Wagner S. J.;Ward M.;White R.;Wierzcholska A.;Zacharias M.;Zajczyk A.;Zdziarski A. A.;Zech A.;Zechlin H. S.;Aleksic J.;Antonelli L. A.;Antoranz P.;Backes M.;Barrio J. A.;Bastieri D.;Becerra Gonzalez J.;Bednarek W.;Berdyugin A.;Berger K.;Bernardini E.;Biland A.;Blanch O.;Bock R. K.;Boller A.;Bonnoli G.;Tridon D. Borla;Braun I.;Bretz T.;Canellas A.;Carmona E.;Carosi A.;Colin P.;Colombo E.;Contreras J. L.;Cortina J.;Cossio L.;Covino S.;Dazzi F.;De Angelis A.;De Cea del Pozo E.;De Lotto B.;Delgado Mendez C.;Diago Ortega A.;Doert M.;Dominguez A.;Prester D. Dominis;Dorner D.;Doro M.;Elsaesser D.;Ferenc D.;Fonseca M. V.;Font L.;Fruck C.;Garcia Lopez R. J.;Garczarczyk M.;Garrido D.;Giavitto G.;Godinovic N.;Hadasch D.;Haefner D.;Herrero A.;Hildebrand D.;Hoehne Moench D.;Hose J.;Hrupec D.;Huber B.;Jogler T.;Klepser S.;Kraehenbuehl T.;Krause J.;La Barbera A.;Lelas D.;Leonardo E.;Lindfors E.;Lombardi S.;Lopez M.;Lorenz E.;Makariev M.;Maneva G.;Mankuzhiyil N.;Mannheim K.;Maraschi L.;Mariotti M.;Martinez M.;Mazin D.;Meucci M.;Miranda J. M.;Mirzoyan R.;Miyamoto H.;Moldon J.;Moralejo A.;Munar P.;Nieto D.;Nilsson K.;Orito R.;Oya I.;Paneque D.;Paoletti R.;Pardo S.;Paredes J. M.;Partini S.;Pasanen M.;Pauss F.;Perez Torres M. A.;Persic M.;Peruzzo L.;Pilia M.;Pochon J.;Prada F.;PRADA MORONI, PIER GIORGIO;Prandini E.;Puljak I.;Reichardt I.;Reinthal R.;Rhode W.;Ribo M.;Rico J.;Ruegamer S.;Saggion A.;Saito K.;Saito T. Y.;Salvati M.;Satalecka K.;Scalzotto V.;Scapin V.;Schultz C.;Schweizer T.;Shayduk M.;SHORE, STEVEN NEIL;Sillanpaa A.;Sitarek J.;Sobczynska D.;Spanier F.;Spiro S.;Stamerra A.;Steinke B.;Storz J.;Strah N.;Suric T.;Takalo L.;Takami H.;Tavecchio F.;Temnikov P.;Terzic T.;Tescaro D.;Teshima M.;Thom M.;Tibolla O.;Torres D. F.;Treves A.;Vankov H.;Vogler P.;Wagner R. M.;Weitzel Q.;Zabalza V.;Zandanel F.;Zanin R.;Arlen T.;Aune T.;Beilicke M.;Benbow W.;Bouvier A.;Bradbury S. M.;Buckley J. H.;Bugaev V.;Byrum K.;Cannon A.;Cesarini A.;Ciupik L.;Connolly M. P.;Cui W.;Dickherber R.;Duke C.;Errando M.;Falcone A.;Finley J. P.;Finnegan G.;Fortson L.;Furniss A.;Galante N.;Gall D.;Godambe S.;Griffin S.;Grube J.;Gyuk G.;Hanna D.;Holder J.;Huan H.;Hui C. M.;Kaaret P.;Karlsson N.;Kertzman M.;Khassen Y.;Kieda D.;Krawczynski H.;Krennrich F.;Lang M. J.;LeBohec S.;Maier G.;McArthur S.;McCann A.;Moriarty P.;Mukherjee R.;Nunez P. D.;Ong R. A.;Orr M.;Otte A. N.;Park N.;Perkins J. S.;Pichel A.;Pohl M.;Prokoph H.;Ragan K.;Reyes L. C.;Reynolds P. T.;Roache E.;Rose H. J.;Ruppel J.;Schroedter M.;Sembroski G. H.;Sentuerk G. D.;Telezhinsky I.;Tesic G.;Theiling M.;Thibadeau S.;Varlotta A.;Vassiliev V. V.;Vivier M.;Wakely S. P.;Weekes T. C.;Williams D. A.;Zitzer B.;de Almeida U. Barres;Cara M.;Casadio C.;Cheung C. C.;McConville W.;Davies F.;Doi A.;Giovannini G.;Giroletti M.;Hada K.;Hardee P.;Harris D. E.;Junor W.;Kino M.;Lee N. P.;Ly C.;Madrid J.;Massaro F.;Mundell C. G.;Nagai H.;Perlman E. S.;Steele I. A.;Walker R. C.;Wood D. L.
2012-01-01
Abstract
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.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11568/155890
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.
