The june 2008 flare of Markarian 421 from optical to TeV energies



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Antoranz Canales, Pedro and Barrio Uña, Juan Abel and Contreras González, José Luis and Fonseca González, Mª Victoria and Miranda Pantoja, José Miguel and Nieto, Daniel (2009) The june 2008 flare of Markarian 421 from optical to TeV energies. Astrophysical journal letters, 691 (1). L13-L19. ISSN 2041-8205

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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.

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© The American Astronomical Society. AGILE is a mission of ASI, with co-participation of INAF and INFN. This work was partially supported by ASI grants I/R/045/04, I/089/06/0, I/011/07/0 and by the Italian Ministry of University and Research (PRIN 2005025417), (ASDC) I/024/05/1. The MAGIC collaboration thanks the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de Los Muchachos in La Palma and support by the German BMBF and MPG, the Italian INFN and Spanish MCINN is acknowledged. This work was supported by ETH Research Grant TH 34/043, by the Polish MNiSzW Grant N N203 390834, the YIP of the Helmholtz Gemeinschaft, the grant of Georgian National Science Foundation GNSF/ST07/4180. E. K. acknowledges financial support from the NCS grant No. 96-2811-M-008-058. The VERITAS collaboration is supported by grants from the U.S. Department of Energy, the National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, Science Foundation Ireland, and PPARC in the UK. We acknowledge the technical support staff at the FLWO. We also acknowledge the Swift Team for carrying out the ToO observation.

Uncontrolled Keywords:BL-Lacertae Objects, X-Ray-Spectra, Magic Telescope, LAC Objects, Gamma-Rays, XMM-Newton, Blazars, Webt, Outburst, Campaign.
Subjects:Sciences > Physics > Electronics
Sciences > Physics > Electricity
Sciences > Physics > Nuclear physics
ID Code:23043
Deposited On:10 Oct 2013 12:03
Last Modified:10 Dec 2018 14:58

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