New Chandra observations of the jet in 3C273. I. Softer X-ray than radio spectra and the X-ray emission mechanism

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dc.creatorJester, S.
dc.creatorHarris, D. E.
dc.creatorMarshall, H. L.
dc.creatorMeisenheimer, K.
dc.date2006-05-20
dc.date.accessioned2026-07-07T11:25:36Z
dc.date.available2026-07-07T11:25:36Z
dc.descriptionThe jet in 3C273 is a high-power quasar jet with radio, optical and X-ray emission whose size and brightness allow a detailed study of the emission processes acting in it. We present deep Chandra observations of this jet and analyse the spectral properties of the jet emission from radio through X-rays. We find that the X-ray spectra are significantly softer than the radio spectra in all regions of the bright part of the jet except for the first bright "knot A", ruling out a model in which the X-ray emission from the entire jet arises from beamed inverse-Compton scattering of cosmic microwave background photons in a single-zone jet flow. Within two-zone jet models, we find that a synchrotron origin for the jet's X-rays requires fewer additional assumptions than an inverse-Compton model, especially if velocity shear leads to efficient particle acceleration in jet flows.
dc.description11 pages, 5 figures, emulateapj. Accepted by ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0605529
dc.identifierhttp://arxiv.org/abs/astro-ph/0605529
dc.identifierAstrophys.J.648:900-909,2006
dc.identifierdoi:10.1086/505962
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/195560
dc.subjectAstrophysics
dc.titleNew Chandra observations of the jet in 3C273. I. Softer X-ray than radio spectra and the X-ray emission mechanism
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