학술논문
Very High Energy outburst of Markarian 501 in May 2009
Document Type
Working Paper
Author
Aliu, E.; Archambault, S.; Archer, A.; Arlen, T.; Aune, T.; Barnacka, A.; Behera, B.; Beilicke, M.; Benbow, W.; Berger, K.; Bird, R.; Bouvier, A.; Böttcher, M.; Buchovecky, M.; Buckley, J. H.; Bugaev, V.; Cardenzana, J. V; Cerruti, M.; Cesarini, A.; Chen, X.; Ciupik, L.; Collins-Hughes, E.; Connolly, M. P.; Cui, W.; Dumm, J.; Eisch, J. D.; Falcone, A.; Federici, S.; Feng, Q.; Finley, J. P.; Fleischhack, H.; Fortin, P.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gillanders, G. H.; Griffin, S.; Griffiths, S. T.; Grube, J.; Gyuk, G.; Hütten, M.; Håkansson, N.; Holder, J.; Hughes, G.; Humensky, T. B.; Johnson, C. A.; Kaaret, P.; Kar, P.; Kelley-Hoskins, N.; Kertzman, M.; Khassen, Y.; Kieda, D.; Krause, M.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Madhavan, A. S; Maier, G.; McArthur, S.; McCann, A.; Meagher, K.; Millis, J.; Moriarty, P.; Mukherjee, R.; Nieto, D.; de Bhróithe, A. O'Faoláin; Ong, R. A.; Orr, M.; Otte, A. N.; Pandel, D.; Park, N.; Pelassa, V.; Perkins, J. S.; Pichel, A.; Pohl, M.; Popkow, A.; Quinn, J.; Ragan, K.; Reyes, L. C.; Reynolds, P. T.; Roache, E.; Rousselle, J.; Rovero, A. C.; Saxon, D. B.; Sembroski, G. H.; Shahinyan, K.; Sheidaei, F.; Skole, C.; Smith, A. W.; Staszak, D.; Telezhinsky, I.; Theiling, M.; Todd, N. W.; Tucci, J. V.; Tyler, J.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wakely, S. P.; Weiner, O. M.; Weinstein, A.; Welsing, R.; Wilhelm, A.; Williams, D. A.; Zitzer, B.; Baring, M. G.; Gónzalez, J. Becerra; Cillis, A. N.; Horan, D.; Paneque, D.
Source
A&A 594, A76 (2016)
Subject
Language
Abstract
The very high energy (VHE; E $>$ 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54938--54956), 2009, as part of an extensive multi-wavelength campaign from radio to VHE. Strong VHE $\gamma$-ray activity was detected on May 1st with Whipple and VERITAS, when the flux (E $>$ 400 GeV) increased to 10 times the pre-flare baseline flux ($3.9{\times 10^{-11}}~{\rm ph~cm^{-2}~s^{-1}}$), reaching five times the flux of the Crab Nebula. This coincided with a decrease in the optical polarization and a rotation of the polarization angle by 15$^{\circ}$. This VHE flare showed a fast flux variation with an increase of a factor $\sim$4 in 25 minutes, and a falling time of $\sim$50 minutes. We present the observations of the quiescent state previous to the flare and of the high state after the flare, focusing on the flux and spectral variability from Whipple, VERITAS, Fermi-LAT, RXTE, and Swift combined with optical and radio data.
Comment: 13 pages, 10 figures. Accepted for publication in Astronomy and Astrophysics
Comment: 13 pages, 10 figures. Accepted for publication in Astronomy and Astrophysics