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Astron. Astrophys. 360, 99-106 (2000)
The jet of 3C 273 observed with ROSAT HRI *
H.-J. Röser 1,
K. Meisenheimer 1,
M. Neumann 1,
R.G. Conway 2 and
R.A. Perley 3
1 Max-Planck-Institut für Astronomie, 69117 Heidelberg, Germany
2 University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire SK11 9DL, UK
3 National Radio Astronomy Observatory, P.O. Box 0, Soccoro, NM 87801, USA
Received 31 March 2000 / Accepted 24 May 2000
Abstract
ROSAT HRI observations of 3C 273 reveal X-ray emission all
along the optically visible jet with the peak of emission at the inner
end. Whereas the X-ray emission from the innermost knot A is
consistent with a continuation of the radio-to-optical synchrotron
continuum, a second population of particles with higher maximum energy
has to be invoked to explain the X-ray emission from knots B, C and D
in terms of synchrotron radiation. Inverse Compton emission could
account for the X-ray flux from the hot spot. We detect a faint X-ray
halo with a characteristic scale of 29 kpc and particle density
on the order of ![[FORMULA]](img1.gif)
m-3,
higher than previously thought.
Key words: acceleration of
particles 
radiation mechanisms:
non-thermal
galaxies:
active
galaxies: jets
galaxies: quasars: individual: 3C 273
* Based on observations with the ROSAT X-ray satellite and also on data collected with the VLA (The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.) and at the European Southern Observatory, Chile (ESO No 51-2-021).
Send offprint requests to: H.-J. Röser (roeser@mpia-hd.mpg.de)
Contents
- 1. Introduction
- 2. The jet of 3C 273 at radio to optical wavelengths
- 3. ROSAT observations
- 4. Origin of the X-ray emission
- 5. The X-ray halo of 3C 273
- 6. Conclusions
- Acknowledgements
- References
© European Southern Observatory (ESO) 2000
Online publication: July 27, 2000
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