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|Title:||H.E.S.S. discovery of very high energy γ -ray emission from PKS 0625-354|
|Other Titles:||H.E.S.S. discovery of very high energy gamma -ray emission from PKS 0625-354|
Ait Benkhali, F.
Becker Tjus, J.
|Citation:||Monthly Notices of the Royal Astronomical Society, 2018; 476(3):4187-4198|
|Publisher:||Oxford University Press|
|H.E.S.S. Collaboration, H. Abdalla ... R. Blackwell ... P. deWilt ... J. Hawkes ... J. Lau ... N. Maxted ... G. Rowell ... F. Voisin ... et al.|
|Abstract:||PKS 0625−354 (z = 0.055) was observed with the four High Energy Stereoscopic System (H.E.S.S.) telescopes in 2012 during 5.5 h. The source was detected above an energy threshold of 200 GeV at a significance level of 6.1σ. No significant variability is found in these observations. The source is well described with a power-law spectrum with photon index Γ = 2.84 ± 0.50stat ± 0.10syst and normalization (at E0 = 1.0 TeV) N0(E0) = (0.58 ± 0.22stat ± 0.12syst) × 10−12 TeV⁻¹ cm⁻² s⁻¹. Multiwavelength data collected with Fermi-LAT, Swift-XRT, Swift-UVOT, ATOM and WISE are also analysed. Significant variability is observed only in the Fermi-LAT γ-ray and Swift-XRT X-ray energy bands. Having a good multiwavelength coverage from radio to very high energy, we performed a broad-band modelling from two types of emission scenarios. The results from a one zone lepto-hadronic and a multizone leptonic models are compared and discussed. On the grounds of energetics, our analysis favours a leptonic multizone model. Models associated to the X-ray variability constraint support previous results, suggesting a BL Lac nature of PKS 0625−354 with, however, a large-scale jet structure typical of a radio galaxy.|
|Keywords:||Radiation mechanisms: non-thermal; galaxies: active; galaxies: individual: PKS 0625−354; galaxies: jets; gamma-rays: galaxies|
|Description:||Advance Access publication 2018 February 20|
|Rights:||© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society|
|Appears in Collections:||Aurora harvest 8|
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