3C 247 has line emission extending for over 10 arcsec along the radio
axis (Fig. 5; see also McCarthy et al. 1995). The inner approximately
2 arcsec radius of the line emission is almost symmetrical, with an
intermediate velocity FWHM and a velocity profile which again may be
consistent with a mean rotational motion or with infall/outflow of
material. Further to the north-east there is a smooth transition into a
region of [O II] emission redshifted by 150 km s^-1^ and with a lower
velocity width. This second region has an associated continuum object,
and it seems likely that what is seen here is an interaction of the
radio galaxy with a companion. The radio galaxy itself shows a
significant 4000 A break of strength 1.61 +/- 0.06; bearing in mind that
the true strength of this break is diluted by aligned continuum
emission, the host galaxy must contain a well-evolved stellar
population. A strong CaK 3933 A absorption feature is readily apparent
in the red-arm spectrum (Fig. 5b).
3C 247 (z=0.7489; Fig. 12).--This is a complex object with several objects or
components within the central few arcseconds. These lie along the radio axis
and are probably associated with a group or cluster centered on 3C 247.
3C 247(z = 0.749; Fig. 33).-Imaging of this galaxy is made difficult by
the presence of a bright star only 4" to the northeast. Our [O II] image
reveals an elongated structure oriented to the northeast, the direction
of the radio source. The [O II] morphology of this object is quite
similar to that of 3C 352. The continuum image was taken with the KPNO 4
m telescope by Djorgovski and Spinrad. While this image is contaminated
by the star, the galaxy appears to be elongated in the same direction as
the [O II] emission. The radio source is a moderately asymmetric 12.5"
double (Jenkins et al. 1977).
1056+432, 3C247, galaxy: Our very sensitive map shows the extended
double-lobed structure as seen in VLA maps (Liu et al. 1992). However,
more details of the substructure within the lobes are seen due to much
higher resolution of our map. The radio core seen at 5 GHz by Liu et al.,
is not detected in our map, indicating a core spectral index of <= 0.2.
The radio structure of 3C247 shows signs of an X-shaped structure. A core
of 3.5 mJy at 5 GHz, also detected by Laing & Kiley (private
communication), lies 1.5 arcsec south-west of the optical identification
- the difference between the radio and optical positions is not
significant. Liu & Pooley (1991b) discuss the [O III] line-emission gas,
which is associated with the galaxy and is extended along the radio
source. The spatial coincidence suggests a connection between the
presence of the dense ionized gas and the distorted shape of the radio
source. The continuous spectral steepening along the distorted arms XW
and YZ is consistent with the idea that the faint emission in regions W
and Z is backflow from the hotspots X and Y respectively.