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Abramowski A., Acero F., Aharonian Felix, Akhperjanian A. G., Anton G., Balzer A., Barnacka A., Barres de Almeida U., Becherini Y., Becker Jürgen, Behera B., Benbow W., Bernlöhr K., Bochow A., Boisson Catherine, Bolmont J., Bordas P., Bouteilier T., Brucker J., Brun F., Brun P., Bulik Tomasz, Büsching I., Carrigan S., Casanova S., Cerruti Matteo, Chadwick Paula, Charbonnier A., Chaves R. C. G., Cheesebrough A., Chounet L.-M., Clapson A.-C., Coignet G., Cologna G., Colom Pierre, Conrad J., Coudreau Nicole, Dalton M., Daniel M.K., Davids I. D., Degrange B., Deil C., Dickinson H. J., Djannati-Ataï Arache, Domainko W., Drury L. O.'C., Dubois F., Dubus G., Dutson K., Dyks J., Dyrda M., Edwards P., Egberts K., Eger P., Espigat Pierre, Fallon L., Farnier C., Fegan S., Feinstein F., Fernandes M. V., Fiasson A., Fontaine G., Förster A., Füßling M., Gallant Y. A., Gast H., Gaylard M. J., Gérard L., Gerbig D., Giebels B., Glicenstein J.-F., Glück B., Goret P., Göring D., Häffner S., Hague J. D., Hampf D., Hauser M., Heinz S., Heinzelmann G., Henri G., Hermann G., Hinton J. A., Hoffmann A., Hofmann W., Hofvergerg 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., Khélifi Bruno, Klein M., Klochkov D., Kluznika W., Kneiske Tanja, Komin Nu., Kosack K., Kossakowski R., Kubanek P., Laffon H., Lamanna G., Lennarz D., Lenain J.-P., Lohse T., Lopatin A., Lu C.-C., Marandon V., Marcowith Alexandre, Martin Jean-Michel, Masbou J., Maurin D., Maxted N., McComb T. J. L., Medina M. C., Méhault J., Melady G., Nguyen N., Moderski R., Monard B., Moulin E., Naumann C. L., Naumann-Godo M., De Naurois M., Nedbal D., Nekrassov D., Nicholas B., Niemiec J., Nolan S. J., Ohm S., De Oña Wilhelmi E., Opitz B., Ostrowski M., Oya I., Panter M., Paz Arribas M., Pedaletti G., Pelletier Guy, Petrucci Pierre-Olivier, Pita Santiago, Pühlhofer G., Punch Michael, Quirrenbach Andreas, 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 Cameron, Ruppel J., Ryde F., Sahakian V., Santangelo Andrea, Schlickeiser R., Schöck F. M., Schulz A., Schwanke U., Schwarzburg S., Schwemmer S., Sikora Marek, Skilton J. L., Sol Hélène, Spengler G., Stawarz L., Steenkamp R., Stegmann C., Stinzing F., Stycz K., Sushch I., Szostek A., Tavernet J.-P., Terrier R., Tluczykont M., Tzioumis Anastasios K., Valerius K., Van Eldik C., Vasileiadis G., Venter C., Venter L., Vialle J. P., Viana A., Vincent P., Völk 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 Andreas, Zechlin H.-S., H.E.S.S. Collaboration

A multiwavelength view of the flaring state of PKS 2155-304 in 2006

Astronomy and Astrophysics, 2012, vol. 539, pp. 149

Référence ADS : 2012A&A...539A.149A

Résumé :

Context. Multiwavelength (MWL) observations of the blazar PKS 2155-304 during two weeks in July and August 2006, the period when two exceptional flares at very high energies (VHE, E ≳ 100 GeV) occurred, provide a detailed picture of the evolution of its emission. The complete data set from this campaign is presented, including observations in VHE γ-rays (H.E.S.S.), X-rays (RXTE, Chandra, Swift XRT), optical (Swift UVOT, Bronberg, Watcher, ROTSE), and in the radio band (NRT, HartRAO, ATCA). Optical and radio light curves from 2004 to 2008 are compared to the available VHE data from this period, to put the 2006 campaign into the context of the long-term evolution of the source.

Aims. The data set offers a close view of the evolution of the source on different time scales and yields new insights into the properties of the emission process. The predictions of synchrotron self-Compton (SSC) scenarios are compared to the MWL data, with the aim of describing the dominant features in the data down to the hour time scale.

Methods. The spectral variability in the X-ray and VHE bands is explored and correlations between the integral fluxes at different wavelengths are evaluated. SSC modelling is used to interpret the general trends of the varying spectral energy distribution.

Results. The X-ray and VHE γ-ray emission are correlated during the observed high state of the source, but show no direct connection with longer wavelengths. The long-term flux evolution in the optical and radio bands is found to be correlated and shows that the source reaches a high state at long wavelengths after the occurrence of the VHE flares. Spectral hardening is seen in the Swift XRT data.

Conclusions. The nightly averaged high-energy spectra of the non-flaring nights can be reproduced by a stationary one-zone SSC model, with only small variations in the parameters. The spectral and flux evolution in the high-energy band during the night of the second VHE flare is modelled with multi-zone SSC models, which can provide relatively simple interpretations for the hour time-scale evolution of the high-energy emission, even for such a complex data set. For the first time in this type of source, a clear indication is found for a relation between high activity at high energies and a long-term increase in the low frequency fluxes.

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