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dc.contributor.authorMarshall, Herman L.
dc.contributor.authorGelbord, Jonathan M.
dc.contributor.authorWorrall, Diana M.
dc.contributor.authorBirkinshaw, Mark
dc.contributor.authorSchwartz, Daniel A.
dc.contributor.authorJauncey, David L.
dc.contributor.authorGriffiths, G.
dc.contributor.authorMurphy, David W.
dc.contributor.authorLovell, James E.J.
dc.contributor.authorPerlman, Eric S.
dc.date.accessioned2018-09-14T18:23:57Z
dc.date.available2018-09-14T18:23:57Z
dc.date.issued2018-03-20
dc.identifier.citationMarshall, H. L., Gelbord, J. M., Worrall, D. M., Birkinshaw, M., Schwartz, D. A., Jauncey, D. L., . . . Godfrey, L. (2018). An X-ray imaging survey of quasar jets: The complete survey. Astrophysical Journal, 856(1) doi:10.3847/1538-4357/aaaf66en_US
dc.identifier.urihttp://hdl.handle.net/11141/2579
dc.description.abstractWe present Chandra X-ray imaging of a flux-limited sample of flat spectrum radio-emitting quasars with jet-like structure. X-rays are detected from 59% of 56 jets. No counter-jets were detected. The core spectra are fitted by power-law spectra with a photon index Γx, whose distribution is consistent with a normal distribution, with a mean of 1.61⁺⁰∙⁰⁴₋₀.₀₅ and dispersion of 0.15⁺⁰∙⁰⁴₋₀.₀₃. We show that the distribution of α ᵣₓ, the spectral index between the X-ray and radio band jet fluxes, fits a Gaussian with a mean of 0.974 ±0.012 and dispersion of 0.077 ±0.008. We test the model in which kiloparsec-scale X-rays result from inverse Compton scattering of cosmic microwave background photons off the jet's relativistic electrons (the IC-CMB model). In the IC-CMB model, a quantity Q computed from observed fluxes and the apparent size of the emission region depends on redshift as (1 + z)³⁺^α. We fit Q ∝ (1 + z)ᵃ, finding a = 0.88 ±0.90, and reject at 99.5% confidence the hypothesis that the average α ᵣₓ depends on redshift in the manner expected in the IC-CMB model. This conclusion is mitigated by a lack of detailed knowledge of the emission region geometry, which requires deeper or higher resolution X-ray observations. Furthermore, if the IC-CMB model is valid for X-ray emission from kiloparsec-scale jets, then the jets must decelerate on average: bulk Lorentz factors should drop from about 15 to 2-3 between parsec and kiloparsec scales. Our results compound the problems that the IC-CMB model has in explaining the X-ray emission of kiloparsec-scale jets.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is made available in accordance with publisher’s policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/3.0/en_US
dc.titleAn X-Ray Imaging Survey of Quasar Jets: The Complete Surveyen_US
dc.typeOtheren_US
dc.identifier.doi10.3847/1538-4357/aaaf66


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