A Multiwavelength View Of The Kiloparsec-scale Jet In 3c273

Details A Multiwavelength View Of The Kiloparsec-scale Jet In 3c273 A Multiwavelength View Of The Kiloparsec-scale Jet In 3c273

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0705u&link_type=abstract

American Astronomical Society, HEAD meeting #9, #7.05; Bulletin of the American Astronomical Society, Vol. 38, p.350

Astronomy and Astrophysics

Astronomy

Scientific paper

Our multiwavelength analysis of the kiloparsec-scale jet in the well-known quasar 3C273 offers new clues to the controversial origin of the X-ray emission seen in many quasar jets. Spitzer IRAC 3.6 and 5.8 micron images of 3C273, combined with HST ACS, Chandra ACIS, and VLA images, show a collimated sequence of bright knots between 13" and 23" from the quasar core. In the infrared, as in the radio, the knots are brightest toward the far end of the jet. In contrast, the strongest X-ray emission comes from the first knot, with subsequent knots getting fainter along the jet. The spectral energy distribution of the first, X-ray-brightest knot shows clearly that the infrared emission is the high-frequency extension of the radio-synchrotron component, while at least half the optical emission from the knot is associated with the X-ray component. Given the similarity between the radio and optical polarization of 3C273 (although the latter has not yet been measured for this specific knot), the SED suggests the X-rays are produced by the synchrotron process rather than inverse-Compton scattering of CMB photons. Sensitive, spatially-resolved polarization measurements of the knot are needed to confirm this conclusion.

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