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Astron. Astrophys. 360, 99-106 (2000)

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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


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] 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)

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© European Southern Observatory (ESO) 2000

Online publication: July 27, 2000