Contents of: VI/111/./abstract/FMACCHET_PROP_4.abs

The following document lists the file abstract/FMACCHET_PROP_4.abs from catalogue VI/111.
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We  propose to carry out infrared imaging of a selected sample of radio
sources with bright radio jets. The existence of high energy electrons,
which are  radiating at  IR and optical wavelengths, puts strong limits
on the particles acceleration  and  energy dissipation within the jets.
A better  understanding of these issues is fundamental to exploring the
connection between the jet, the nuclear energy source, the interstellar
medium and the large scale radio emission.
The search  for the optical counterparts to radio jets has lead to only
a few detections;  this  indicates that the break frequency of the jets
synchrotron  emission  is  typically  < 10^14 erg. In addition, optical
emission  from the  jets has  the disadvantage  of being diluted by the
starlight near the galactic nuclei.
Infrared  observations  are particularly suited for this study; in fact
the  emission  from the galaxy is strongly suppressed, and the infrared
emission  corresponds  to  break  frequencies  more  than  an  order of
magnitude smaller than those accessible with optical observations.
High spatial  resolution and sensitivity in the infrared are needed for
such an investigation, which is uniquely suited to ISOCAM.
Our proposed study is  also particularly  important in the framework of
the unified models  for radio loud AGN; optical jets have been observed
only in  sources with  one-sided radio-jets  while the  detection of an
optical (or infrared) counter-part  should depend  only on the observed
radio flux  and not on the radio morphology. Infrared observations of a
sample of  radio galaxies containing both one-sided and two-sided radio
jets  is  necessary  to  address  this  issue.  The correlation between
extended radio and infrared emission will also be investigated.

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