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An X-Ray Imaging Survey of Quasar Jets: The Complete Survey

Marshall, H L; Gelbord, J M; Worrall, Diana M; Birkinshaw, Mark; Schwartz, D A; Jauncey, David; Griffiths, G; Murphy, D W; Lovell, J; Perlman, E; Godfrey, Leith

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We 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,...[Show more]

dc.contributor.authorMarshall, H L
dc.contributor.authorGelbord, J M
dc.contributor.authorWorrall, Diana M
dc.contributor.authorBirkinshaw, Mark
dc.contributor.authorSchwartz, D A
dc.contributor.authorJauncey, David
dc.contributor.authorGriffiths, G
dc.contributor.authorMurphy, D W
dc.contributor.authorLovell, J
dc.contributor.authorPerlman, E
dc.contributor.authorGodfrey, Leith
dc.date.accessioned2021-10-19T01:28:10Z
dc.date.available2021-10-19T01:28:10Z
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/251014
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.
dc.description.sponsorshipSupport for this work was provided in part by the National Aeronautics and Space Administration (NASA) through the Smithsonian Astrophysical Observatory (SAO) contract SV3- 73016 to MIT for support of the Chandra X-Ray Center (CXC), which is operated by SAO for and on behalf of NASA under contract NAS8-03060. Support was also provided by NASA under contract NAS 8-39073 to SAO.
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.publisherIOP Publishing
dc.rights© 2018. The American Astronomical Society
dc.rights.urihttps://creativecommons.org/licenses/by/3.0/
dc.sourceThe Astrophysical Journal
dc.titleAn X-Ray Imaging Survey of Quasar Jets: The Complete Survey
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume856
dc.date.issued2018
local.identifier.absfor020104 - Galactic Astronomy
local.identifier.ariespublicationa383154xPUB9667
local.publisher.urlhttp://iopscience.iop.org/
local.type.statusPublished Version
local.contributor.affiliationMarshall, H L, Massachusetts Institute of Technology
local.contributor.affiliationGelbord, J M, Massachusetts Institute of Technology
local.contributor.affiliationWorrall, Diana M, University of Bristol
local.contributor.affiliationBirkinshaw, Mark, University of Bristol
local.contributor.affiliationSchwartz, D A, Harvard-Smithsonian Center for Astrophysics
local.contributor.affiliationJauncey, David, College of Science, ANU
local.contributor.affiliationGriffiths, G, University of Bristol
local.contributor.affiliationMurphy, D W, California Institute of Technology Jet Propulsion Laboratory
local.contributor.affiliationLovell, J, University of Tasmania
local.contributor.affiliationPerlman, E, Florida institute of Technology
local.contributor.affiliationGodfrey, Leith, College of Science, ANU
local.bibliographicCitation.issue66
local.bibliographicCitation.startpage1
local.bibliographicCitation.lastpage25
local.identifier.doi10.3847/1538-4357/aaaf66
dc.date.updated2020-11-23T11:32:48Z
local.identifier.scopusID2-s2.0-85044712064
dcterms.accessRightsOpen Access
dc.provenanceOriginal content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
dc.rights.licenseCC Attribution 3.0 License
CollectionsANU Research Publications

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