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 RID G-6769-2011 RID B-5372-2009 RID A-2903-2010

SHORE, STEVEN NEIL;
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.
2009
Donnarumma, I; Vittorini, V; Vercellone, S; Del Monte, E; Feroci, M; D'Ammando, F; Pacciani, L; Chen, Aw; Tavani, M; Bulgarelli, A; Giuliani, A; Longo, F; Pucella, G; Argan, A; Barbiellini, G; Boffelli, F; Caraveo, P; Cattaneo, Pw; Cocco, V; Costa, E; De Paris, G; Di Cocco, G; Evangelista, Y; Fiorini, M; Froysland, T; Frutti, M; Fuschino, F; Galli, M; Gianotti, F; Labanti, C; Lapshov, I; Lazzarotto, F; Lipari, P; Marisaldi, M; Mastropietro, M; Mereghetti, S; Morelli, E; Morselli, A; Pellizzoni, A; Perotti, F; Picozza, P; Porrovecchio, G; Prest, M; Rapisarda, M; Rappoldi, A; Rubini, A; Soffitta, P; Trifoglio, M; Trois, A; Vallazza, E; Zambra, A; Zanello, D; Pittori, C; Santolamazza, P; Verrecchia, F; Giommi, P; Colafrancesco, S; Salotti, L; Villata, M; Raiteri, Cm; Chen, Wp; Efimova, Nv; Jordan, B; Konstantinova, Ts; Koptelova, E; Kurtanidze, Om; Larionov, Vm; Ros, Ja; Sadun, Ac; Anderhub, H; Antonelli, La; Antoranz, P; Backes, M; Baixeras, C; Balestra, S; Barrio, Ja; Bartko, H; Bastieri, D; Gonzalez, Jb; Becker, Jk; Bednarek, W; Berger, K; Bernardini, E; Biland, A; Bock, Rk; Bonnoli, G; Bordas, P; Tridon, Db; Bosch Ramon, V; Bretz, T; Britvitch, I; Camara, M; Carmona, E; Chilingarian, A; Commichau, S; Contreras, Jl; Cortina, J; Costado, Mt; Covino, S; Curtef, V; Dazzi, F; De Angelis, A; Del Pozo, Ed; Reyes, Rd; De Lotto, B; De Maria, M; De Sabata, F; Mendez, Cd; Dominguez, A; Dorner, D; Doro, M; Elsaesser, D; Errando, M; Ferenc, D; Fernandez, E; Firpo, R; Fonseca, Mv; Font, L; Galante, N; Lopez, Rjg; Garczarczyk, M; Gaug, M; Goebel, F; Hadasch, D; Hayashida, M; Herrero, A; Hohne Monch, D; Hose, J; Hsu, Cc; Huber, S; Jogler, T; Kranich, D; La Barbera, A; Laille, A; Leonardo, E; Lindfors, E; Lombardi, S; Lopez, M; Lorenz, E; Majumdar, P; Maneva, G; Mankuzhiyil, N; Mannheim, K; Maraschi, L; Mariotti, M; Martinez, M; Mazin, D; Meucci, M; Meyer, M; Miranda, Jm; Mirzoyan, R; Moldon, J; Moles, M; Moralejo, A; Nieto, D; Nilsson, K; Ninkovic, J; Oya, I; Paoletti, R; Paredes, Jm; Pasanen, M; Pascoli, D; Pauss, F; Pegna, Rg; Perez Torres, Ma; Persic, M; Peruzzo, L; Prada, F; Prandini, E; Puchades, N; Raymers, A; Rhode, W; Ribo, M; Rico, J; Rissi, M; Robert, A; Rugamer, S; Saggion, A; Saito, Ty; Salvati, M; Sanchez Conde, M; Sartori, P; Satalecka, K; Scalzotto, V; Scapin, V; Schweizer, T; Shayduk, M; Shinozaki, K; Shore, STEVEN NEIL; Sidro, N; Sierpowska Bartosik, A; Sillanpaa, A; Sitarek, J; Sobczynska, D; Spanier, F; Stamerra, A; Stark, Ls; Takalo, L; Tavecchio, F; Temnikov, P; Tescaro, D; Teshima, M; Tluczykont, M; Torres, Df; Turini, N; Vankov, H; Venturini, A; Vitale, V; Wagner, Rm; Wittek, W; Zabalza, V; Zandanel, F; Zanin, R; Zapatero, J; Acciari, V; Aliu, E; Arlen, T; Beilicke, M; Benbow, W; Bradbury, Sm; Buckley, Jh; Bugaev, V; Butt, Y; Byrum, K; Cannon, A; Cesarini, A; Chow, Yc; Ciupik, L; Cogan, P; Colin, P; Cui, W; Daniel, Mk; Dickherber, R; Duke, C; Ergin, T; Fegan, Sj; Finley, Jp; Finnegan, G; Fortin, P; Furniss, A; Gall, D; Gillanders, Gh; Guenette, R; Gyuk, G; Grube, J; Hanna, D; Holder, J; Horan, D; Hui, Cm; Humensky, Tb; Imran, A; Kaaret, P; Karlsson, N; Kertzman, M; Kieda, D; Kildea, J; Konopelko, A; Krawczynski, H; Krennrich, F; Lang, Mj; Lebohec, S; Maier, G; Mccann, A; Mccutcheon, M; Milovanovic, A; Moriarty, P; Nagai, T; Ong, Ra; Otte, An; Pandel, D; Perkins, Js; Pichel, A; Pohl, M; Ragan, K; Reyes, Lc; Reynolds, Pt; Roache, E; Rose, Hj; Schroedter, M; Sembroski, Gh; Smith, Aw; Steele, D; Swordy, Sp; Theiling, M; Toner, Ja; Valcarcel, L; Varlotta, A; Wakely, Sp; Ward, Je; Weekes, Tc; Weinstein, A; Williams, Da; Wissel, S; Wood, M; Zitzer, B.
File in questo prodotto:
Non ci sono file associati a questo prodotto.

I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.

Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11568/128076
 Attenzione

Attenzione! I dati visualizzati non sono stati sottoposti a validazione da parte dell'ateneo

Citazioni
  • ???jsp.display-item.citation.pmc??? ND
  • Scopus ND
  • ???jsp.display-item.citation.isi??? 90
social impact