As one of the brightest active blazars in both X-ray and very high energy γ-ray bands, Mrk 501, is very useful for physics associated with jets from active galactic nuclei. The ARGO-YBJ experiment has monitoredMrk 501 for γ-rays above 0.3 TeV since 2007 November. The largest flare since 2005 was observed from 2011 October and lasted until about 2012 April. In this paper, a detailed analysis of this event is reported. During the brightest γ-ray flaring episodes from 2011 October 17 to November 22, an excess of the event rate over 6σ is detected by ARGO-YBJ in the direction of Mrk 501, corresponding to an increase of the γ -ray flux above 1 TeV by a factor of 6.6 ± 2.2 from its steady emission. In particular, the γ -ray flux above 8 TeV is detected with a significance better than 4σ. Based on time-dependent synchrotron self-Compton (SSC) processes, the broadband energy spectrum is interpreted as the emission from an electron energy distribution parameterized with a single power-law function with an exponential cutoff at its high-energy end. The average spectral energy distribution for the steady emission is well described by this simple one-zone SSC model. However, the detection of γ -rays above 8 TeV during the flare challenges this model due to the hardness of the spectra. Correlations between X-rays and γ -rays are also investigated.

B. Bartoli, BERNARDINI, P., X. J. Bi, C. Bleve, I. Bolognino, P. Branchini, et al. (2012). LONG-TERM MONITORING OF MRK 501 FOR ITS VERY HIGH ENERGYγ EMISSION AND A FLARE IN 2011 OCTOBER. THE ASTROPHYSICAL JOURNAL, 758(1) [10.1088/0004-637X/758/1/2].

LONG-TERM MONITORING OF MRK 501 FOR ITS VERY HIGH ENERGYγ EMISSION AND A FLARE IN 2011 OCTOBER

MARSELLA, GIOVANNI;
2012-01-01

Abstract

As one of the brightest active blazars in both X-ray and very high energy γ-ray bands, Mrk 501, is very useful for physics associated with jets from active galactic nuclei. The ARGO-YBJ experiment has monitoredMrk 501 for γ-rays above 0.3 TeV since 2007 November. The largest flare since 2005 was observed from 2011 October and lasted until about 2012 April. In this paper, a detailed analysis of this event is reported. During the brightest γ-ray flaring episodes from 2011 October 17 to November 22, an excess of the event rate over 6σ is detected by ARGO-YBJ in the direction of Mrk 501, corresponding to an increase of the γ -ray flux above 1 TeV by a factor of 6.6 ± 2.2 from its steady emission. In particular, the γ -ray flux above 8 TeV is detected with a significance better than 4σ. Based on time-dependent synchrotron self-Compton (SSC) processes, the broadband energy spectrum is interpreted as the emission from an electron energy distribution parameterized with a single power-law function with an exponential cutoff at its high-energy end. The average spectral energy distribution for the steady emission is well described by this simple one-zone SSC model. However, the detection of γ -rays above 8 TeV during the flare challenges this model due to the hardness of the spectra. Correlations between X-rays and γ -rays are also investigated.
2012
B. Bartoli, BERNARDINI, P., X. J. Bi, C. Bleve, I. Bolognino, P. Branchini, et al. (2012). LONG-TERM MONITORING OF MRK 501 FOR ITS VERY HIGH ENERGYγ EMISSION AND A FLARE IN 2011 OCTOBER. THE ASTROPHYSICAL JOURNAL, 758(1) [10.1088/0004-637X/758/1/2].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10447/466614
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