Physics
Scientific paper
Jun 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004phdt........20r&link_type=abstract
PHD Thesis, Jodrell Bank Observatory, University of Manchester, 207 pages
Physics
Jets, Jet, 3C273, 3C78, 3C15, 3C346
Scientific paper
The jets of 3C15, 3C78, 3C273 and 3C346 were observed with the Very Large Array and Multi Element Radio Linked Interferometer Network at radio wavelengths and the Hubble Space Telescope at IR to UV wavelengths as part of a multiwavelength study of extragalactic jets with a focus on their UV emission. The observations within this work represent the deepest and highest resolutions of these objects to date and when convolved to a common resolution allow the derivation of the radio to optical spectra of the individual regions and knots.
All the jets were found to be spatially resolved across their width and consist of a number of bright hotspots. The optical and UV emission was observed to be coincident with the radio features of all four jets with only knot A of 3C273 displaying any positional offset. A ballistic modelling of the jet of 3C346 was performed and reproduced the large scale jet features including the amplitude and wavelength of the observed curvature with jet axis precession periods of 30,000 years and velocities around 0.7c.
The synchrotron spectra of the various regions were computed for 3C78, 3C273 and 3C346 and a number of spectral fits performed using the standard single injection and continuous injection spectral models. The physical conditions within these regions were calculated assuming minimum energy considerations, with magnetic fields of 1-100 nT, pressures of 0.05-1 nPa and corresponding electron radiative lifetimes of the order of hundreds to thousands of years. We find one can reconcile the the difference between the electron lifetime and the light travel for the optical components by invoking a relativistic jet flow of bulk Lorentz factor, Gamma>2, and a jet inclination of 2.5-30 degrees.
Both 3C78 and 3C273 show a flattening of the spectra around the UV and although this flattening has been previously reported for 3C273 the spectral flattening of the first knot of 3C78 represents the first detection of such a break for this source. 3C346 displays no such break although only a single knot located around the bend in the jet is observed at UV wavelengths.
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