Very high energy outburst of Markarian 501 in May 2009

The VERITAS Collaboration

Research output: Contribution to journalArticle

10 Citations (Scopus)

Abstract

The very high energy (VHE; E> 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54 938-54 956), 2009, as part of an extensive multi-wavelength campaign from radio to VHE. Strong VHE γ-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 × 10-11 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°. This VHE flare showed a fast flux variation with an increase of a factor ∼4 in 25 min, and a falling time of ∼50 min. 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.

Original languageEnglish (US)
Article numberA76
JournalAstronomy and Astrophysics
Volume594
DOIs
StatePublished - Oct 1 2016

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outburst
polarization
flares
radio
energy
crab
wavelength
Crab nebula
optical polarization
X Ray Timing Explorer
falling
rays
wavelengths

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

@article{0c08c165e576496ba3b356a59f219a5e,
title = "Very high energy outburst of Markarian 501 in May 2009",
abstract = "The very high energy (VHE; E> 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54 938-54 956), 2009, as part of an extensive multi-wavelength campaign from radio to VHE. Strong VHE γ-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 × 10-11 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°. This VHE flare showed a fast flux variation with an increase of a factor ∼4 in 25 min, and a falling time of ∼50 min. 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.",
author = "{The VERITAS Collaboration} and E. Aliu and S. Archambault and A. Archer and T. Arlen and T. Aune and A. Barnacka and B. Behera and M. Beilicke and W. Benbow and K. Berger and R. Bird and M. B{\"o}ttcher and A. Bouvier and M. Buchovecky and Buckley, {J. H.} and V. Bugaev and Cardenzana, {J. V.} and M. Cerruti and A. Cesarini and X. Chen and L. Ciupik and E. Collins-Hughes and Connolly, {M. P.} and W. Cui and J. Dumm and Eisch, {J. D.} and A. Falcone and S. Federici and Q. Feng and Finley, {J. P.} and H. Fleischhack and Falcone, {Abraham David} and L. Fortson and A. Furniss and N. Galante and D. Gall and Gillanders, {G. H.} and S. Griffin and Griffiths, {S. T.} and J. Grube and G. Gyuk and M. H{\"u}tten and N. H{\aa}kansson and J. Holder and G. Hughes and Humensky, {T. B.} and Johnson, {C. A.} and P. Kaaret and P. Kar and N. Kelley-Hoskins",
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Very high energy outburst of Markarian 501 in May 2009. / The VERITAS Collaboration.

In: Astronomy and Astrophysics, Vol. 594, A76, 01.10.2016.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Very high energy outburst of Markarian 501 in May 2009

AU - The VERITAS Collaboration

AU - Aliu, E.

AU - Archambault, S.

AU - Archer, A.

AU - Arlen, T.

AU - Aune, T.

AU - Barnacka, A.

AU - Behera, B.

AU - Beilicke, M.

AU - Benbow, W.

AU - Berger, K.

AU - Bird, R.

AU - Böttcher, M.

AU - Bouvier, A.

AU - Buchovecky, M.

AU - Buckley, J. H.

AU - Bugaev, V.

AU - Cardenzana, J. V.

AU - Cerruti, M.

AU - Cesarini, A.

AU - Chen, X.

AU - Ciupik, L.

AU - Collins-Hughes, E.

AU - Connolly, M. P.

AU - Cui, W.

AU - Dumm, J.

AU - Eisch, J. D.

AU - Falcone, A.

AU - Federici, S.

AU - Feng, Q.

AU - Finley, J. P.

AU - Fleischhack, H.

AU - Falcone, Abraham David

AU - Fortson, L.

AU - Furniss, A.

AU - Galante, N.

AU - Gall, D.

AU - Gillanders, G. H.

AU - Griffin, S.

AU - Griffiths, S. T.

AU - Grube, J.

AU - Gyuk, G.

AU - Hütten, M.

AU - Håkansson, N.

AU - Holder, J.

AU - Hughes, G.

AU - Humensky, T. B.

AU - Johnson, C. A.

AU - Kaaret, P.

AU - Kar, P.

AU - Kelley-Hoskins, N.

PY - 2016/10/1

Y1 - 2016/10/1

N2 - The very high energy (VHE; E> 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54 938-54 956), 2009, as part of an extensive multi-wavelength campaign from radio to VHE. Strong VHE γ-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 × 10-11 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°. This VHE flare showed a fast flux variation with an increase of a factor ∼4 in 25 min, and a falling time of ∼50 min. 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.

AB - The very high energy (VHE; E> 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54 938-54 956), 2009, as part of an extensive multi-wavelength campaign from radio to VHE. Strong VHE γ-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 × 10-11 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°. This VHE flare showed a fast flux variation with an increase of a factor ∼4 in 25 min, and a falling time of ∼50 min. 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.

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