We present optical, X-ray, high-energy ((sic) 30 GeV) and very high energy ((sic) 100 GeV; VHE) observations of the high-frequency peaked blazar Mrk 421 taken between 2008 May 24 and June 23. A high-energy gamma-ray signal was detected by AGILE with root TS = 4.5 between June 9 and 15, with F(E > 100 MeV) = 42(-12)(+14) x 10(-8) photons cm(-2) s(-1). This flaring state is brighter than the average flux observed by EGRET by a factor of similar to 3, but still consistent with the highest EGRET flux. In hard X-rays (20-60 keV) SuperAGILE resolved a five-day flare (June 9-15) peaking at similar to 55 mCrab. SuperAGILE, RXTE/ASM and Swift/BAT data show a correlated flaring structure between soft and hard X-rays. Hints of the same flaring behavior are also detected in the simultaneous optical data provided by the GASP-WEBT. A Swift/XRT observation near the flaring maximum revealed the highest 2-10 keV flux ever observed from this source, of 2.6 x 10(-9) erg cm(-2) s(-1) (i.e. > 100 mCrab). A peak synchrotron energy of similar to 3 keV was derived, higher than typical values of similar to 0.5-1 keV. VHE observations with MAGIC and VERITAS between June 6 and 8 showed the flux peaking in a bright state, well correlated with the X-rays. This extraordinary set of simultaneous data, covering a 12-decade spectral range, allowed for a deep analysis of the spectral energy distribution as well as of correlated light curves. The gamma-ray flare can be interpreted within the framework of the synchrotron self-Compton model in terms of a rapid acceleration of leptons in the jet.
THE JUNE 2008 FLARE OF MARKARIAN 421 FROM OPTICAL TO TeV ENERGIES / I., Donnarumma; V., Vittorini; S., Vercellone; E. D., Monte; M., Feroci; F., D'Ammando; L., Pacciani; A. W., Chen; M., Tavani; A., Bulgarelli; A., Giuliani; Longo, Francesco; G., Pucella; A., Argan; G., Barbiellini; F., Boffelli; P., Caraveo; P. W., Cattaneo; V., Cocco; E., Costa; G. D., Paris; G. D., Cocco; Y., Evangelista; M., Fiorini; T., Froysland; M., Frutti; F., Fuschino; M., Galli; F., Gianotti; C., Labanti; I., Lapshov; F., Lazzarotto; P., Lipari; M., Marisaldi; M., Mastropietro; S., Mereghetti; E., Morelli; A., Morselli; A., Pellizzoni; F., Perotti; P., Picozza; G., Porrovecchio; M., Prest; M., Rapisarda; A., Rappoldi; A., Rubini; P., Soffitta; M., Trifoglio; A., Trois; E., Vallazza; A., Zambra; D., Zanello; C., Pittori; P., Santolamazza; F., Verrecchia; P., Giommi; S., Colafrancesco; L., Salotti; M., Villata; C. M., Raiteri; W. P., Chen; N. V., Efimova; B., Jordan; T. S., Konstantinova; E., Koptelova; O. M., Kurtanidze; V. M., Larionov; J. A., Ros; A. C., Sadun; H., Anderhub; L. A., Antonelli; P., Antoranz; M., Backes; C., Baixeras; S., Balestra; J. A., Barrio; H., Bartko; D., Bastieri; J. B., Gonzalez; J. K., Becker; W., Bednarek; K., Berger; E., Bernardini; A., Biland; R. K., Bock; G., Bonnoli; P., Bordas; D. B., Tridon; V., Bosch Ramon; T., Bretz; I., Britvitch; M., Camara; E., Carmona; A., Chilingarian; S., Commichau; J. L., Contreras; J., Cortina; M. T., Costado; S., Covino; V., Curtef; F., Dazzi; A. D., Angelis; E. D., Del Pozo; R. D., Reyes; B. D., Lotto; M. D., Maria; F. D., Sabata; C. D., Mendez; A., Dominguez; D., Dorner; M., Doro; D., Elsaesser; M., Errando; D., Ferenc; E., Fernandez; R., Firpo; M. V., Fonseca; L., Font; N., Galante; R. J. G., Lopez; M., Garczarczyk; M., Gaug; F., Goebel; D., Hadasch; M., Hayashida; A., Herrero; D., Hohne Monch; J., Hose; C. C., Hsu; S., Huber; T., Jogler; D., Kranich; A. L., Barbera; A., Laille; E., Leonardo; E., Lindfors; S., Lombardi; M., Lopez; E., Lorenz; P., Majumdar; G., Maneva; N., Mankuzhiyil; K., Mannheim; L., Maraschi; M., Mariotti; M., Martinez; D., Mazin; M., Meucci; M., Meyer; J. M., Miranda; R., Mirzoyan; J., Moldon; M., Moles; A., Moralejo; D., Nieto; K., Nilsson; J., Ninkovic; I., Oya; R., Paoletti; J. M., Paredes; M., Pasanen; D., Pascoli; F., Pauss; R. G., Pegna; M. A., Perez Torres; M., Persic; L., Peruzzo; F., Prada; E., Prandini; N., Puchades; A., Raymers; W., Rhode; M., Ribo; J., Rico; M., Rissi; A., Robert; S., Rugamer; A., Saggion; T. Y., Saito; M., Salvati; M., Sanchez Conde; P., Sartori; K., Satalecka; V., Scalzotto; V., Scapin; T., Schweizer; M., Shayduk; K., Shinozaki; S. N., Shore; N., Sidro; A., Sierpowska Bartosik; A., Sillanpaa; J., Sitarek; D., Sobczynska; F., Spanier; A., Stamerra; L. S., Stark; L., Takalo; F., Tavecchio; P., Temnikov; D., Tescaro; M., Teshima; M., Tluczykont; D. F., Torres; N., Turini; H., Vankov; A., Venturini; V., Vitale; R. M., Wagner; W., Wittek; V., Zabalza; F., Zandanel; R., Zanin; J., Zapatero; V., Acciari; E., Aliu; T., Arlen; M., Beilicke; W., Benbow; S. M., Bradbury; J. H., Buckley; V., Bugaev; Y., Butt; K., Byrum; A., Cannon; A., Cesarini; Y. C., Chow; L., Ciupik; P., Cogan; P., Colin; W., Cui; M. K., Daniel; R., Dickherber; C., Duke; T., Ergin; S. J., Fegan; J. P., Finley; G., Finnegan; P., Fortin; A., Furniss; D., Gall; G. H., Gillanders; R., Guenette; G., Gyuk; J., Grube; D., Hanna; J., Holder; D., Horan; C. M., Hui; T. B., Humensky; A., Imran; P., Kaaret; N., Karlsson; M., Kertzman; D., Kieda; J., Kildea; A., Konopelko; H., Krawczynski; F., Krennrich; M. J., Lang; S., Lebohec; G., Maier; A., Mccann; M., Mccutcheon; A., Milovanovic; P., Moriarty; T., Nagai; R. A., Ong; A. N., Otte; D., Pandel; J. S., Perkins; A., Pichel; M., Pohl; K., Ragan; L. C., Reyes; P. T., Reynolds; E., Roache; H. J., Rose; M., Schroedter; G. H., Sembroski; A. W., Smith; D., Steele; S. P., Swordy; M., Theiling; J. A., Toner; L., Valcarcel; A., Varlotta; S. P., Wakely; J. E., Ward; T. C., Weekes; A., Weinstein; D. A., Williams; S., Wissel; M., Wood; B., Zitzer. - In: THE ASTROPHYSICAL JOURNAL LETTERS. - ISSN 2041-8205. - STAMPA. - 691:(2009), pp. L13-L19. [10.1088/0004-637X/691/1/L13]
THE JUNE 2008 FLARE OF MARKARIAN 421 FROM OPTICAL TO TeV ENERGIES
LONGO, FRANCESCO;
2009-01-01
Abstract
We present optical, X-ray, high-energy ((sic) 30 GeV) and very high energy ((sic) 100 GeV; VHE) observations of the high-frequency peaked blazar Mrk 421 taken between 2008 May 24 and June 23. A high-energy gamma-ray signal was detected by AGILE with root TS = 4.5 between June 9 and 15, with F(E > 100 MeV) = 42(-12)(+14) x 10(-8) photons cm(-2) s(-1). This flaring state is brighter than the average flux observed by EGRET by a factor of similar to 3, but still consistent with the highest EGRET flux. In hard X-rays (20-60 keV) SuperAGILE resolved a five-day flare (June 9-15) peaking at similar to 55 mCrab. SuperAGILE, RXTE/ASM and Swift/BAT data show a correlated flaring structure between soft and hard X-rays. Hints of the same flaring behavior are also detected in the simultaneous optical data provided by the GASP-WEBT. A Swift/XRT observation near the flaring maximum revealed the highest 2-10 keV flux ever observed from this source, of 2.6 x 10(-9) erg cm(-2) s(-1) (i.e. > 100 mCrab). A peak synchrotron energy of similar to 3 keV was derived, higher than typical values of similar to 0.5-1 keV. VHE observations with MAGIC and VERITAS between June 6 and 8 showed the flux peaking in a bright state, well correlated with the X-rays. This extraordinary set of simultaneous data, covering a 12-decade spectral range, allowed for a deep analysis of the spectral energy distribution as well as of correlated light curves. The gamma-ray flare can be interpreted within the framework of the synchrotron self-Compton model in terms of a rapid acceleration of leptons in the jet.Pubblicazioni consigliate
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