![]() | ![]() |
Astron. Astrophys. 338, 840-842 (1998) 4. DiscussionAn EVN+MERLIN map of 3C287 at 5 GHz is presented by Fanti et
al. (1989). They found that the most compact A component - which is
the brightest one - is in the centre of the source. The source
brightness decreases smoothly along the curved jet, and has a
secondary maximum at 15 mas to East and 45 mas to North from
the centre. This component marked with C in their paper. The two point
spectral index between 18 cm and 6 cm
(S The most remarkable difference between the map of Fanti et al.
(1989) and our results is that we cannot find emission above the
3 The near circular track of the jet bridge line suggested earlier by
Fanti et al. 1989 was based on their C component. 1.6 GHz
observations support this regularly curving jet scenario (e.g. Nan et
al. 1988). Unfortunately, we cannot decide whether component C moved
away or faded below our 3 Recent VLBA observations at 8.4 GHz also failed to detect component C (Dallacasa et al. 1998). There is no compact core at a few mJy level even at this frequency. Component f is identified just above the image noise, while component g also appears at about 1 mJy/beam contour level using 7 mas restoring beam (Dallacasa 1998, priv. comm.). ![]() ![]() ![]() ![]() © European Southern Observatory (ESO) 1998 Online publication: September 17, 1998 ![]() |