3C 13. The HST observations of this source show the optical galaxy to
be extended over nearly 4" with two tail-like structures to the south
and east of the nucleus (McCarthy et al. 1997). The extended emission
in both the nucleus and on the 1" scale is aligned with the radio
axis at a P.A. of 145^deg^. Best et al. (1997a, 1998) find that the
infrared emission from the host galaxy is also strongly aligned with
the radio axis. Our radio image shows clear hot spots but no radio
core in this high-redshift source (Fig. 15). More sensitive
observations are required to be able to image the full radio bridge.
3C 13.0 (z=1.351; Fig. 2).--The identification is well detected and is extended
over nearly 4". There are two faint arm or tail-like structures to the south
and east of the nucleus. The radio source is a 28" double oriented in P.A.
145^deg^. The extended emission in both the nucleus and on the 1" scale is
aligned with the radio axis.
3C 13: Identified with a V = 22.5 galaxy with a redshift of z = 1.351
(Spinrad, McCarthy & Strauss, unpublished). Loss of data resulting in
relatively poor image quality precluded the detection of a radio core.
Red 200-inch (1.5m) plate shows a number of faint galaxies
within 25 arcsec, possibly a distant cluster.
A deeper red (Eastman 127-04) plate has been published by
Smith, H.E., Burbidge, E.M., and Spinrad, H.
(1976) Ap. J., 210, 627
who suggest one of these as a candidate;
but it is 10 arcsec from radio position of
Adgie, R.L., and Gent, H.
(1966) Nature, 209, 549
in the general direction of the 5C 003 source position angle
(1969) MNRAS, 144, 101.
Hence the position agreement is only marginal and is further confused
by radio positions that are discrepant (23 arcsec difference between
5C 003 and position from
Macdonald, G.H., Kenderdine, S., and Neville, A.C.
(1968) MNRAS, 138, 259.
The average of the radio positions by Adgie and Gent and
by Macdonald et al. is shown as a cross;
the Smith et al. suggestion, by bars.