Insights into the HE gamma-ray emission of Markarian 501 in the Fermi era PDF Print
Image
Spectral energy distribution for Mrk 501 averaged over all observations taken during the multifrequency campaign performed between 2009 March 15 (MJD 54905) and 2009 August 1 (MJD 55044). See Figure 8 below for further details.

Reference:  A. A. Abdo et al.,  Astrophysical Journal 727: 129, 2011 (Fermi-LAT, VERITAS, GASP-WEBT & multi-wavelength partners)

Full text version here

ArXiv version: ArXiV:1011.5260

Contact person: Daniel Gall

 

We report on the γ-ray activity of the blazar Mrk 501 during the first 480 days of Fermi operation. We find that the average LAT γ-ray spectrum of Mrk501 can be well described by a single power-law function with a photon index of 1.78±0.03. While we observe relatively mild flux variations with the Fermi-LAT (within less than a factor of 2), we detect remarkable spectral variability where the hardest observed spectral index within the LAT energy range is 1.52 ± 0.14, and the softest one is 2.51 ± 0.20. These unexpected spectral changes do not correlate with the measured flux variations above 0.3 GeV. In this paper, we also present the first results from the 4.5-month-long multifrequency campaign (2009 March 15 – August 1) on Mrk501, which included the VLBA, Swift, RXTE, MAGIC and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent time and energy coverage of the source throughout the entire campaign. The extensive radio to TeV data set from this campaign provides us with the most detailed spectral energy distribution yet collected for this source during its relatively low activity. The average spectral energy distribution of Mrk501 is well described by the standard one-zone syn- chrotron self-Compton model. In the framework of this model, we find that the dominant emission region is characterized by a size ~0.1 pc (comparable within a factor of few to the size of the partially-resolved VLBA core at 15-43 GHz), and that the total jet power (≃ 1044 erg s−1) constitutes only a small fraction (∼ 10−3) of the Eddington luminosity. The energy distribution of the freshly-accelerated radiating electrons required to fit the time-averaged data has a broken power-law form in the energy range 0.3 GeV−10 TeV, with spectral indices 2.2 and 2.7 below and above the break energy of 20 GeV. We argue that such a form is consistent with a scenario in which the bulk of the energy dissipation within the dominant emission zone of Mrk 501 is due to relativistic, proton-mediated shocks. We find that the ultrarelativistic electrons and mildly relativistic protons within the blazar zone, if comparable in number, are in approximate energy equipartition, with their energy dominating the jet magnetic field energy by about two orders of magnitude.

 

Figures from paper (click to get full size image):

 

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Figure 7: Spectral energy distribution for Mrk 501 from Fermi -LAT for several time intervals of interest. The panel (a) shows the SED for the time period before the multifrequency campaign (MJD 54683–54901), the panel (b) for the time interval corresponding to the multifrequency campaign (MJD 54905–55044) and the panel (c) for the period after the campaign (MJD 55044–55162). In all panels, the black line depicts the result of the unbinned likelihood power-law fit, the red contours denote the 68% uncertainty of the power-law fit and blue arrows denote upper limits at 95% confidence level, which were computed for the differential energy ranges with a signal of TS

 

 

 

 

 

 

 

 

 

 

Last Updated on Saturday, 09 July 2011 06:40
 

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