MULTIWAVELENGTH OBSERVATIONS OF A TeV-FLARE FROM W COMAE

Acciari, V. A.; Aliu, E.; Aune, T.; Beilicke, M.; Benbow, W.; Böttcher, M.; Boltuch, D.; Buckley, J. H.; Bradbury, S. M.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Ciupik, L.; Cogan, P.; Cui, Wei; Dickherber, R.; Duke, C.; Falcone, A.; Finley, J. P.; Fortin, P.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guénette, R.; Gyuk, G.; Hanna, D.; Holder, J.; Hui, C. M.; Humensky, T. B.; Kaaret, Philip; Karlsson, N.; Kertzman, M.; Kieda, D.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Maier, G.; McArthur, S.; McCann, A.; McCutcheon, M.; Millis, J.; Moriarty, P.; Ong, R. A.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Pichel, A.; Pohl, M.; Quinn, J.; Ragan, K.; Reyes, Luis; Reynolds, P. T.; Roache, E.; Rose, H. J.; Sembroski, G. H.; Smith, A. W.; Steele, D.; Theiling, M.; Thibadeau, S.; Varlotta, A.; Vassiliev, V. V.; Vincent, Stéphane; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A. J.R.; Weisgarber, T.; Williams, D. A.; Wissel, S.; Wood, M.; Pian, E.; Vercellone, S.; Donnarumma, I.; D’Ammando, F.; Bulgarelli, A.; Chen, Andrew; Giuliani, A.; Longo, F.; Pacciani, L.; Pucella, G.; Vittorini, V.; Tavani, M.; Argan, A.; Barbiellini, G.; Caraveo, P. A.; Cattaneo, P. W.; Cocco, V.; Costa, E.; Monte, E. Del; Paris, G. De; Cocco, G. Di; Evangelista, Y.; Feroci, M.; Fiorini, M.; Froysland, T.; Frutti, M.; Fuschino, F.; Galli, M.; Gianotti, F.; Labanti, C.; Lapshov, I.; Lazzarotto, F.; Lipari, P.; Marisaldi, M.; Mastropietro, Michele; Mereghetti, S.; Morelli, E.; Morselli, A.; Pellizzoni, A.; Perotti, F.; Piano, G.; Picozza, P.; Pilia, M.; Porrovecchio, G.; Prest, M.; Rapisarda, M.; Rappoldi, A.; Rubini, A.; Sabatini, S.; 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, C. M.; Aller, H. D.; Aller, M. F.; Архаров, А. А.; Ефимова, Н. В.; Larionov, V. M.; Leto, P.; Ligustri, R.; Lindfors, E.; Pasanen, M.; Kurtanidze, O. M.; Tetradze, S. D.; Lähteenmäki, A.; Kotiranta, Mikko; Cucchiara, Antonino; Romano, P.; Nesci, R.; Pursimo, T.; Heidt, J.; Benítez, E.; Hiriart, D.; Nilsson, K.; Berdyugin, A.; Mújica, R.; Dultzin, D.; López, J. M.; Mommert, Michael; Sorcia, M.; Pérez, I. de la Calle

doi:10.1088/0004-637x/707/1/612

Cited by 82 publications

(63 citation statements)

References 41 publications

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“…For BL Lacertae objects, the prototype of the BL Lac objects shows that the SSC+ERC model using the BLR emission as seed photons is better than a two-zone SSC model, and the pure SSC model is likely to be ruled out, acting like a FSRQ ). The SSC+ERC model with external IR seed photons can agree with the IDV for 3C 66A (Reyes et al 2011) and gets a more reasonable magnetic field parameter for W Comae (Acciari et al 2009). Actually, no evidence of the thermal emission has been found for S5 0716+714 and 3C 66A.…”

Section: Discussionmentioning

confidence: 86%

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

Liao

Bai

Liu

et al. 2014

ApJ

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S5 0716+714 is a typical BL Lacertae object. In this paper we present the analysis and results of long-term simultaneous observations in the radio, near-infrared, optical, X-ray, and γ -ray bands, together with our own photometric observations for this source. The light curves show that the variability amplitudes in γ -ray and optical bands are larger than those in the hard X-ray and radio bands and that the spectral energy distribution (SED) peaks move to shorter wavelengths when the source becomes brighter, which is similar to other blazars, i.e., more variable at wavelengths shorter than the SED peak frequencies. Analysis shows that the characteristic variability timescales in the 14.5 GHz, the optical, the X-ray, and the γ -ray bands are comparable to each other. The variations of the hard X-ray and 14.5 GHz emissions are correlated with zero lag, and so are the V band and γ -ray variations, which are consistent with the leptonic models. Coincidences of γ -ray and optical flares with a dramatic change of the optical polarization are detected. Hadronic models do not have the same natural explanation for these observations as the leptonic models. A strong optical flare correlating a γ -ray flare whose peak flux is lower than the average flux is detected. The leptonic model can explain this variability phenomenon through simultaneous SED modeling. Different leptonic models are distinguished by average SED modeling. The synchrotron plus synchrotron selfCompton (SSC) model is ruled out because of the extreme input parameters. Scattering of external seed photons, such as the hot-dust or broad-line region emission, and the SSC process are probably both needed to explain the γ -ray emission of S5 0716+714.

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Section: Discussionmentioning

confidence: 86%

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

Liao

Bai

Liu

et al. 2014

ApJ

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“…Alternatively, a flat spectrum can be produced in the hadronic models (e.g., Mannheim 1993;Mücke et al 2003). In more complicated, multi-zone leptonic models, the GeV-TeV emission of a few slightly shifted inverse Compton peaks can also emulate a flat spectrum (e.g., spine-sheath layer model, Tavecchio & Ghisellini 2008, or SSC+EC model used for explaining SED of an IBL object W Com, Acciari et al 2009b). Finally, using the model by Dominguez et al (2010), we find that the change in the spectrum due to the absorption in the extragalactic background light radiation field is within the error of the spectral slope.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

DETECTION OF VERY HIGH ENERGY Γ-Ray EMISSION FROM THE PERSEUS CLUSTER HEAD-TAIL GALAXY IC 310 BY THE MAGIC TELESCOPES

Aleksić¹,

Antonelli²,

Antoranz³

et al. 2010

ApJ

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We report on the detection with the MAGIC telescopes of very high energy (VHE) γ -rays from IC 310, a head-tail radio galaxy in the Perseus galaxy cluster, observed during the interval 2008 November to 2010 February. The Fermi satellite has also detected this galaxy. The source is detected by MAGIC at a high statistical significance of 7.6σ in 20.6 hr of stereo data. The observed spectral energy distribution is flat with a differential spectral index of −2.00 ± 0.14. The mean flux above 300 GeV, between 2009 October and 2010 February, (3.1 ± 0.5) × 10 −12 cm −2 s −1 , corresponds to (2.5 ± 0.4)% of Crab Nebula units. Only an upper limit, of 1.9% of L207 L208 ALEKSIĆ ET AL. Vol. 723Crab Nebula units above 300 GeV, was obtained with the 2008 data. This, together with strong hints (>3σ ) of flares in the middle of 2009 October and November, implies that the emission is variable. The MAGIC results favor a scenario with the VHE emission originating from the inner jet close to the central engine. More complicated models than a simple one-zone synchrotron self-Compton (SSC) scenario, e.g., multi-zone SSC, external Compton, or hadronic, may be required to explain the very flat spectrum and its extension over more than three orders of magnitude in energy.

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“…Observations were made in "wobble" pointing mode (Fomin et al 1994) considering the presence of another TeV source in the field of view (1ES 1218+304, offset 0°.76 from B21215+30), as described in Aliu et al (2013). Data were processed using standard VERITAS analysis pipelines (Acciari et al 2009;Archambault et al 2013). The energy threshold of the analysis is 200 GeV, with a systematic uncertainty of 20% on the energy estimation.…”

Section: Veritas Observationsmentioning

confidence: 99%

A Luminous and Isolated Gamma-Ray Flare from the Blazar B2 1215+30

Abeysekara¹,

Archambault²,

Archer³

et al. 2017

ApJ

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B21215+30 is a BL-Lac-type blazar that was first detected at TeV energies by the MAGIC atmospheric Cherenkov telescopes and subsequently confirmed by the Very Energetic Radiation Imaging Telescope Array System (VERITAS) observatory with data collected between 2009 and 2012. In 2014 February 08, VERITAS detected a large-amplitude flare from B21215+30 during routine monitoring observations of the blazar 1ES1218 +304, located in the same field of view. The TeV flux reached 2.4 times the Crab Nebula flux with a variability timescale of <3.6 hr. Multiwavelength observations with Fermi-LAT, Swift, and the Tuorla Observatory revealed a correlated high GeV flux state and no significant optical counterpart to the flare, with a spectral energy distribution where the gamma-ray luminosity exceeds the synchrotron luminosity. When interpreted in the framework of a onezone leptonic model, the observed emission implies a high degree of beaming, with Doppler factor d > 10, and an electron population with spectral index < p 2.3.

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MULTIWAVELENGTH OBSERVATIONS OF A TeV-FLARE FROM W COMAE

Cited by 82 publications

References 41 publications

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

DETECTION OF VERY HIGH ENERGY Γ-Ray EMISSION FROM THE PERSEUS CLUSTER HEAD-TAIL GALAXY IC 310 BY THE MAGIC TELESCOPES

A Luminous and Isolated Gamma-Ray Flare from the Blazar B2 1215+30

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