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- W3208732945 abstract "We present a model for the broadband radio-to-$gamma$-ray spectral energy distribution of the compact radio source, PKS 1718-649. Because of its young age (100 years) and proximity ($z=0.014$), PKS 1718-649 offers a unique opportunity to study nuclear conditions and the jet/host galaxy feedback process at the time of an initial radio jet expansion. PKS 1718-649 is one of a handful of young radio jets with $gamma$-ray emission confirmed with the Fermi/LAT detector. We show that this $gamma$-ray emission can be successfully explained by Inverse Compton scattering of the ultraviolet photons, presumably from an accretion flow, off non-thermal 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 infrared photons emitted by a cold gas in the vicinity of the expanding radio lobes contributes significantly to the X-ray band, the data require that an additional X-ray emission mechanism is at work, e.g. a weak X-ray corona or a radiatively inefficient accretion flow, 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, $L_j simeq 2.2 times 10^{42}$ erg s$^{-1}$, and expands in an environment with density $n_0 simeq 20$ cm$^{-3}$. The inferred mass accretion rate and gas mass reservoir within 50-100 pc are consistent with estimates from the literature obtained by tracing molecular gas in the innermost region of the host galaxy with SINFONI and ALMA." @default.
- W3208732945 created "2021-11-08" @default.
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- W3208732945 date "2022-12-01" @default.
- W3208732945 modified "2023-09-26" @default.
- W3208732945 title "The Origin of High-energy Emission in the Young Radio Source PKS 1718–649" @default.
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- W3208732945 doi "https://doi.org/10.3847/1538-4357/ac98ba" @default.
- W3208732945 hasPublicationYear "2022" @default.
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