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The December 2009 gamma-ray flare of 3C 454.3: the multifrequency campaign | | L. Pacciani
; V. Vittorini
; M. Tavani
; M. T. Fiocchi
; S. Vercellone
; F. D'Ammando
; T. Sakamoto
; E. Pian
; C. M. Raiteri
; M. Villata
; M. Sasada
; R. Itoh
; M. Yamanaka
; M. Uemura
; E. Striani
; D. Fugazza
; A. Tiengo
; H. A. Krimm
; M. C. Stroh
; A. D. Falcone
; P. A. Curran
; A. C. Sadun
; A. Lahteenmaki
; M. Tornikoski
; H. D. Aller
; M. F. Aller
; C. S. Lin
; V. M. Larionov
; P. Leto
; L. O. Takalo
; A. Berdyugin
; M. A. Gurwell
; A. Bulgarelli
; A. W. Chen
; I. Donnarumma
; A. Giuliani
; F. Longo
; G. Pucella
; A. Argan
; G. Barbiellini P. Caraveo
; P. W. Cattaneo
; V. Cocco
; E. Costa
; G. De Paris
; E. Del Monte
; G. Di Cocco
; Y. Evangelista
; A. Ferrari
; M. Feroci
; M. Fiorini
; F. Fuschino
; M. Galli
; F. Gianotti
; C. Labanti
; I. Lapshov
; F. Lazzarotto
; P. Lipari
; M. Marisaldi
; S. Mereghetti
; E. Morelli
; E. Moretti
; A. Morselli
; A. Pellizzoni
; F. Perotti
; G. Piano
; P. Picozza
; M. Pilia
; M. Prest
; M. Rapisarda
; A. Rappoldi
; A. Rubini
; S. Sabatini
; P. Soffitta
; M. Trifoglio
; A. Trois
; E. Vallazza
; D. Zanello
; S. Colafrancesco
; C. Pittori
; F. Verrecchia
; P. Santolamazza
; F. Lucarelli
; P. Giommi
; L. Salotti
; | | Date: |
18 May 2010 | | Abstract: | During the month of December, 2009 the blazar 3C 454.3 became the brightest
gamma-ray source in the sky, reaching a peak flux F ~2000E-8 ph/cm2/s for E >
100 MeV. Starting in November, 2009 intensive multifrequency campaigns
monitored the 3C 454 gamma-ray outburst. Here we report the results of a
2-month campaign involving AGILE, INTEGRAL, Swift/XRT, Swift/BAT, RossiXTE for
the high-energy observations, and Swift/UVOT, KANATA, GRT, REM for the
near-IR/optical/UV data. The GASP/WEBT provided radio and additional optical
data. We detected a long-term active emission phase lasting ~1 month at all
wavelengths: in the gamma-ray band, peak emission was reached on December 2-3,
2009. Remarkably, this gamma-ray super-flare was not accompanied by
correspondingly intense emission in the optical/UV band that reached a level
substantially lower than the previous observations in 2007-2008. The lack of
strong simultaneous optical brightening during the super-flare and the
determination of the broad-band spectral evolution severely constrain the
theoretical modelling. We find that the pre- and post-flare broad-band behavior
can be explained by a one-zone model involving SSC plus external Compton
emission from an accretion disk and a broad-line region. However, the spectra
of the Dec. 2-3, 2009 super-flare and of the secondary peak emission on Dec. 9,
2009 cannot be satisfactorily modelled by a simple one-zone model. An
additional particle component is most likely active during these states. | | Source: | arXiv, 1005.3263 | | Services: | Forum | Review | PDF | Favorites | |
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