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Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195)

Published online by Cambridge University Press:  01 August 2006

D. A. Schwartz ,
D. E. Harris ,
H. Landt ,
A. Siemiginowska ,
E. S. Perlman ,
C. C. Cheung ,
J. M. Gelbord ,
D. M. Worrall ,
M. Birkinshaw  and
S. G. Jorstad
...Show all authors
D. A. Schwartz
Affiliation:
Smithsonian Astrophysical Observatory, Cambridge MA 02138, USA email: das@cfa.harvard.edu
D. E. Harris
Affiliation:
Smithsonian Astrophysical Observatory, Cambridge MA 02138, USA email: das@cfa.harvard.edu
H. Landt
Affiliation:
Smithsonian Astrophysical Observatory, Cambridge MA 02138, USA email: das@cfa.harvard.edu
A. Siemiginowska
Affiliation:
Smithsonian Astrophysical Observatory, Cambridge MA 02138, USA email: das@cfa.harvard.edu
E. S. Perlman
Affiliation:
University of Maryland, Baltimore County, Baltimore MD 21250, USA
C. C. Cheung
Affiliation:
NRAO/Stanford University, Palo Alto CA 94305, USA
J. M. Gelbord
Affiliation:
Massachusetts Institute of Technology, Cambridge MA 02139, USA
D. M. Worrall
Affiliation:
Physics Department, University of Bristol, Bristol BS8 1TL, UK
M. Birkinshaw
Affiliation:
Physics Department, University of Bristol, Bristol BS8 1TL, UK
S. G. Jorstad
Affiliation:
Institute for Astrophysical Research, Boston University, Boston MA 02215, USA
A. P. Marscher
Affiliation:
Institute for Astrophysical Research, Boston University, Boston MA 02215, USA
L. Stawarz
Affiliation:
Kavli Inst. for Particle Astroph. and Cosmology, Stanford Univ., Stanford CA 94305, USA
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Abstract

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We investigate the variations of the magnetic field, Doppler factor, and relativistic particle density along the jet of a quasar at z=0.72. We chose 4C 19.44 for this study because of its length and straight morphology. The 18 arcsec length of the jet provides many independent resolution elements in the Chandra X-ray image. The straightness suggests that geometry factors, although uncertain, are almost constant along the jet. We assume the X-ray emission is from inverse Compton scattering of the cosmic microwave background. With the aid of assumptions about jet alignment, equipartition between magnetic-field and relativistic-particle energy, and filling factors, we find that the jet is in bulk relativistic motion with a Doppler factor ≈ 6 at an angle no more than 10∘ to the line of sight over de-projected distances ≈ 150–600 kpc from the quasar, and with a magnetic field ≈10 μGauss.

Keywords

(Galaxies:) quasars: individual (4C 19.44, PKS 1354+135) – galaxies: jets – X-rays
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 443 - 444
Copyright
Copyright © International Astronomical Union 2007

References

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