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H.E.S.S. detection of very high-energy gamma-ray emission from the quasar PKS 0736+017

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cris.lastimport.scopus2024-02-12T20:37:29Z
dc.abstract.enContext. 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 r<SUB>BLR</SUB> with a bulk Lorentz factor Γ ≃ 20, or at the level of the radius of the dusty torus r<SUB>torus</SUB> 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.
dc.affiliationUniwersytet Warszawski
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dc.date.accessioned2024-01-25T03:05:11Z
dc.date.available2024-01-25T03:05:11Z
dc.date.copyright2019-11-12
dc.date.issued2020
dc.description.accesstimeBEFORE_PUBLICATION
dc.description.financePublikacja bezkosztowa
dc.description.versionORIGINAL_AUTHOR
dc.description.volume633
dc.identifier.doi10.1051/0004-6361/201935906
dc.identifier.issn0004-6361
dc.identifier.urihttps://repozytorium.uw.edu.pl//handle/item/108396
dc.identifier.weblinkhttp://adsabs.harvard.edu/abs/2020A&A...633A.162H
dc.languageeng
dc.pbn.affiliationastronomy
dc.relation.ispartofAstronomy and Astrophysics
dc.relation.pagesA162
dc.rightsOther
dc.sciencecloudnosend
dc.titleH.E.S.S. detection of very high-energy gamma-ray emission from the quasar PKS 0736+017
dc.typeJournalArticle
dspace.entity.typePublication