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dc.contributor.authorPerlman, Eric S.
dc.contributor.authorMeyer, Eileen T.
dc.contributor.authorGeorganopoulos, Markos
dc.contributor.authorSparks, William B.
dc.contributor.authorGodfrey, Leith E H
dc.contributor.authorLovell, James E J
dc.date.accessioned2015-09-14T18:46:35Z
dc.date.available2015-09-14T18:46:35Z
dc.date.issued2015-06-01
dc.identifier.citationMeyer, E. T., Georganopoulos, M., Sparks, W. B., Godfrey, L., Lovell, J. E., & Perlman, E. (2015). Ruling out IC/CMB X-rays in PKS 0637-752 and the Implications for TeV Emission from Large-scale Quasar Jets. The Astrophysical Journal, 805(2), 154.en_US
dc.identifier.urihttp://hdl.handle.net/11141/747
dc.description.abstractThe Chandra X-ray observatory has discovered dozens of resolved, kiloparsec-scale jets associated with powerful quasars in which the X-ray fluxes are observed to be much higher than the expected level based on the radio-optical synchrotron spectrum. The most popular explanation for the anomalously high and hard X-ray fluxes is that these jets do not decelerate significantly by the kiloparsec scale, but rather remain highly relativistic (Lorentz factors ). By adopting a small angle to the line of sight, the X-rays can thus be explained by inverse Compton upscattering of cosmic microwave background (CMB) photons (IC/CMB), where the observed emission is strongly Doppler boosted. Using over six years of Fermi monitoring data, we show that the expected hard, steady gamma-ray emission implied by the IC/CMB model is not seen in PKS 0637-752, the prototype jet for which this model was first proposed. IC/CMB emission is thus ruled out as the source of the X-rays, joining recent results for the jets in 3C 273 (using the same method) and PKS 1136-135 (using UV polarization). We further show that the Fermi observations give an upper limit of δ < 6.5 for the four brightest X-ray knots of PKS 0637-752, and derive an updated limit of δ < 7.8 for knots A and B1 of 3C 273 (assuming equipartition). Finally, we discuss the fact that high levels of synchrotron X-ray emission in a slow jet will unavoidably lead to a level of angle-integrated TeV emission which exceeds that of the TeV BL Lac class.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is available in accordance with the publisher's policy. It may be subject to copyright law.en_US
dc.rights.urihttp://iopscience.iop.org/0004-637X/page/Copyright%20and%20permissionsen_US
dc.titleRuling out IC/CMB X-rays in PKS 0637-752 and the implications for TEV emission from large-scale quasar jetsen_US
dc.typeArticleen_US
dc.identifier.doi10.1088/0004-637X/805/2/154


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