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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7168
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dc.contributor.authorMondal, Samaresh-
dc.contributor.authorGupta, Nayantara-
dc.date.accessioned2019-02-28T19:25:23Z-
dc.date.available2019-02-28T19:25:23Z-
dc.date.issued2019-01-
dc.identifier.citationAstroparticle Physics, 2019, Vol.107, p15-21en_US
dc.identifier.issn0927-6505-
dc.identifier.urihttp://hdl.handle.net/2289/7168-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractRadio observations by ALMA and upper limits on gamma-ray flux by Fermi LAT have ruled out inverse Compton scattering of Cosmic Microwave Background radiation by relativistic electrons (IC/CMB) as the origin of X-ray emission from extended jets of six quasars 3C 273, PKS 0637-752, PKS 1136-135, PKS 1229-021, PKS 1354+195, and PKS 2209+080. Here we consider two populations of accelerated electrons in each knot of the extended jets to explain the radio to optical and the X-ray emission by synchrotron cooling of relativistic electrons. In all cases, the jet power required is lower than the Eddington’s luminosity and the observed knot emissions are well explained in this scenario.en_US
dc.language.isoenen_US
dc.publisherElsevier B.V.en_US
dc.relation.urihttps://ui.adsabs.harvard.edu//#abs/2019APh...107...15M/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1811.06422en_US
dc.relation.urihttps://doi.org/10.1016/j.astropartphys.2018.11.002en_US
dc.rights2019, Elsevier B.Ven_US
dc.subjectQuasarsen_US
dc.subjectX-raysen_US
dc.subjectjetsen_US
dc.titleA two population electron synchrotron model for knots of extended jetsen_US
dc.typeArticleen_US
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