dc.contributor.author | Schwartz, D. A. | |
dc.contributor.author | Murphy, D. W. | |
dc.contributor.author | Lovell, J. E. J. | |
dc.contributor.author | Worrall, D. M. | |
dc.contributor.author | Birkinshaw, M. | |
dc.contributor.author | Perlman, E. S. | |
dc.contributor.author | Godfrey, L. E. H. | |
dc.contributor.author | Jauncey, D. L. | |
dc.contributor.author | Gelbord, Jonathan | |
dc.contributor.author | Marshall, Herman | |
dc.date.accessioned | 2015-02-27T16:52:59Z | |
dc.date.available | 2015-02-27T16:52:59Z | |
dc.date.issued | 2011-03 | |
dc.date.submitted | 2010-05 | |
dc.identifier.issn | 0067-0049 | |
dc.identifier.issn | 1538-4365 | |
dc.identifier.uri | http://hdl.handle.net/1721.1/95735 | |
dc.description.abstract | We present results from continued Chandra X-ray imaging and spectroscopy of a flux-limited sample of flat spectrum radio-emitting quasars with jet-like extended structure. X-rays are detected from 24 of the 39 jets observed so far. We compute the distribution of α [subscript rx], the spectral index between the X-ray and radio bands, showing that it is broad, extending at least from 0.8 to 1.2. While there is a general trend that the radio brightest jets are detected most often, it is clear that predicting the X-ray flux from the radio knot flux densities is risky, so a shallow X-ray survey is the most effective means for finding jets that are X-ray bright. We test the model in which the X-rays result from inverse Compton (IC) scattering of cosmic microwave background (CMB) photons by relativistic electrons in the jet moving with a high bulk Lorentz factor nearly along the line of sight. Depending on how the jet magnetic fields vary with z, the observed X-ray to radio flux ratios do not follow the redshift dependence expected from the IC-CMB model. For a subset of our sample with known superluminal motion based on VLBI observations, we estimate the angle of the kiloparsec-scale jet to the line of sight by considering the additional information in the bends observed between parsec- and kiloparsec-scale jets. These angles are sometimes much smaller than estimates based on the IC-CMB model with a Lorentz factor of 15, indicating that these jets may decelerate significantly from parsec scales to kiloparsec scales. | en_US |
dc.description.sponsorship | Chandra X-ray Center (U.S.) (Grant GO4-5124X) | en_US |
dc.language.iso | en_US | |
dc.publisher | IOP Publishing | en_US |
dc.relation.isversionof | http://dx.doi.org/10.1088/0067-0049/193/1/15 | en_US |
dc.rights | Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. | en_US |
dc.source | American Astronomical Society | en_US |
dc.title | AN X-RAY IMAGING SURVEY OF QUASAR JETS: TESTING THE INVERSE COMPTON MODEL | en_US |
dc.type | Article | en_US |
dc.identifier.citation | Marshall, H. L., J. M. Gelbord, D. A. Schwartz, D. W. Murphy, J. E. J. Lovell, D. M. Worrall, M. Birkinshaw, E. S. Perlman, L. Godfrey, and D. L. Jauncey. “An X-Ray IMAGING SURVEY OF QUASAR JETS: TESTING THE INVERSE COMPTON MODEL.” The Astrophysical Journal Supplement Series 193, no. 1 (March 1, 2011): 15. © The American Astronomical Society | en_US |
dc.contributor.department | MIT Kavli Institute for Astrophysics and Space Research | en_US |
dc.contributor.mitauthor | Marshall, Herman Lee | en_US |
dc.contributor.mitauthor | Gelbord, Jonathan | en_US |
dc.relation.journal | The Astrophysical Journal. Supplement Series | en_US |
dc.eprint.version | Final published version | en_US |
dc.type.uri | http://purl.org/eprint/type/JournalArticle | en_US |
eprint.status | http://purl.org/eprint/status/PeerReviewed | en_US |
dspace.orderedauthors | Marshall, H. L.; Gelbord, J. M.; Schwartz, D. A.; Murphy, D. W.; Lovell, J. E. J.; Worrall, D. M.; Birkinshaw, M.; Perlman, E. S.; Godfrey, L.; Jauncey, D. L. | en_US |
mit.license | PUBLISHER_POLICY | en_US |
mit.metadata.status | Complete | |