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dc.contributor.authorSobolewska, Małgosia
dc.contributor.authorMigliori, Giulia
dc.contributor.authorOstorero, Luisa
dc.contributor.authorSiemiginowska, Aneta
dc.contributor.authorStawarz, Łukasz
dc.contributor.authorGuainazzi, Matteo
dc.contributor.authorHardcastle, Martin J.
dc.date.accessioned2023-09-22T08:00:02Z
dc.date.available2023-09-22T08:00:02Z
dc.date.issued2022-12-12
dc.identifier.citationSobolewska , M , Migliori , G , Ostorero , L , Siemiginowska , A , Stawarz , Ł , Guainazzi , M & Hardcastle , M J 2022 , ' The Origin of High-energy Emission in the Young Radio Source PKS 1718–649 ' , The Astrophysical Journal , vol. 941 , no. 1 , 52 , pp. 1-9 . https://doi.org/10.3847/1538-4357/ac98ba
dc.identifier.issn0004-637X
dc.identifier.otherArXiv: http://arxiv.org/abs/2111.02611v1
dc.identifier.otherJisc: 780066
dc.identifier.otherpublisher-id: apjac98ba
dc.identifier.othermanuscript: ac98ba
dc.identifier.otherother: aas35569
dc.identifier.otherJisc: 868501
dc.identifier.urihttp://hdl.handle.net/2299/26714
dc.description© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. https://creativecommons.org/licenses/by/4.0/
dc.description.abstractWe present a model for the broadband radio-to-γ-ray spectral energy distribution of the compact radio source PKS 1718 − 649. Because of its young age (≃100 yr) and proximity (z = 0.014), PKS 1718 − 649 offers a unique opportunity to study the nuclear conditions and the jet/host galaxy feedback process at the time of the initial radio jet expansion. PKS 1718 − 649 is one of a handful of young radio jets with γ-ray emission that has been confirmed by the Fermi/LAT detector. We show that in PKS1718−649 this γ-ray emission can be successfully explained by Inverse Compton scattering of the UV photons, presumably from an accretion flow, off nonthermal electrons in the expanding radio lobes. The origin of the X-ray emission in PKS 1718 − 649 is more elusive. While Inverse Compton scattering of the IR photons emitted by a cold gas in the vicinity of the expanding radio lobes contributes significantly to the X-ray luminosity, the data require an additional source of X-rays, e.g., a weak X-ray corona or a radiatively inefficient accretion flow, as expected from a LINER-type nucleus, such as that of PKS 1718 − 649. We find that the jet in PKS 1718 − 649 has low power, L j ≃ 2 × 1042 erg s−1, and expands in an environment with density n 0 ≃ 3–20 cm−3. The inferred mass accretion rate and gas mass reservoir within 50–100 pc of the galactic center are consistent with estimates from the literature obtained by tracing molecular gas in the innermost region of the host galaxy with SINFONI and the Atacama Large Millimeter/submillimeter Array.en
dc.format.extent9
dc.format.extent787821
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subject310
dc.subjectGalaxies and Cosmology
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe Origin of High-energy Emission in the Young Radio Source PKS 1718–649en
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.contributor.institutionSPECS Deans Group
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85144575486&partnerID=8YFLogxK
rioxxterms.versionofrecord10.3847/1538-4357/ac98ba
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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