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http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1797| Insights into the high-energy γ -ray emission of markarian 501 from extensive multifrequency observations in the fermi era | |
| Alberto Carramiñana Alonso Luis Carrasco Bazúa | |
| Acceso Abierto | |
| Atribución-NoComercial-SinDerivadas | |
| Acceleration of particles – BL Lacertae objects General – BL Lacertae objects Individual (Mrk 501)– galaxies Active – gamma rays General – radiation mechanisms Non-thermal | |
| 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 Large Area Telescope (LAT) γ -ray spectrum of Mrk 501 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 two), 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) onMrk 501, which included the Very Long Baseline Array (VLBA), Swift, RXTE, MAGIC, and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent temporal 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 Mrk 501 is well described by the standard one-zone synchrotron self-Compton (SSC) 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. | |
| The Astrophysical Journal | |
| 2011-02 | |
| Artículo | |
| Inglés | |
| Estudiantes Investigadores Público en general | |
| Abdo, A. A., et al., (2011), Insights into the high-energy γ -ray emission of markarian 501 from extensive multifrequency observations in the fermi era, The Astrophysical Journal, Vol.727(129): 1-26 | |
| ASTRONOMÍA Y ASTROFÍSICA | |
| Versión aceptada | |
| acceptedVersion - Versión aceptada | |
| Aparece en las colecciones: | Artículos de Astrofísica |
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