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Título: | H.E.S.S. detection of very high-energy γ -ray emission from the quasar PKS 0736+017 |
Autor: | Abdalla, H.; Cerruti, Matteo; Smith, P. S.; H.E.S.S. Collaboration | Palabras clave: | Astroparticle physics Gamma rays: general Quasars: individual: PKS 0736+017 Relativistic processes |
Fecha de publicación: | 28-ene-2020 | Editor: | EDP Sciences | Citación: | Astronomy and Astrophysics 633 (2020) | Resumen: | [Context] Flat-spectrum radio-quasars (FSRQs) are rarely detected at very high energies (E 100 GeV) due to their low-frequency-peaked spectral energy distributions. At present, only six FSRQs are known to emit very high-energy (VHE) photons, representing only 7% of the VHE extragalactic catalog, which is largely dominated by high-frequency-peaked BL Lacertae objects. [Aims] Following the detection of MeV–GeV γ-ray flaring activity from the FSRQ PKS 0736+017 (z = 0.189) with Fermi-LAT, the H.E.S.S. array of Cherenkov telescopes triggered target-of-opportunity (ToO) observations on February 18, 2015, with the goal of studying the γ-ray emission in the VHE band. [Methods] H.E.S.S. ToO observations were carried out during the nights of February 18, 19, 21, and 24, 2015. Together with Fermi-LAT, the multi-wavelength coverage of the flare includes Swift observations in soft X-ray and optical-UV bands, and optical monitoring (photometry and spectro-polarimetry) by the Steward Observatory, and the ATOM, the KAIT, and the ASAS-SN telescopes. [Results] VHE emission from PKS 0736+017 was detected with H.E.S.S. only during the night of February 19, 2015. Fermi-LAT data indicate the presence of a γ-ray flare, peaking at the time of the H.E.S.S. detection, with a flux doubling timescale of around six hours. The γ-ray flare was accompanied by at least a 1 mag brightening of the non-thermal optical continuum. No simultaneous observations at longer wavelengths are available for the night of the H.E.S.S. detection. The γ-ray observations with H.E.S.S. and Fermi-LAT are used to put constraints on the location of the γ-ray emitting region during the flare: it is constrained to be just outside the radius of the broad-line region rBLR with a bulk Lorentz factor Γ ≃ 20, or at the level of the radius of the dusty torus rtorus with Γ ≃ 60. [Conclusions] PKS 0736+017 is the seventh FSRQ known to emit VHE photons, and at z = 0.189 is the nearest so far. The location of the γ-ray emitting region during the flare can be tightly constrained thanks to opacity, variability, and collimation arguments. |
Versión del editor: | http://doi.org/10.1051/0004-6361/201935906 | URI: | http://hdl.handle.net/10261/232873 | DOI: | 10.1051/0004-6361/201935906 | Identificadores: | doi: 10.1051/0004-6361/201935906 issn: 1432-0746 |
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