We present in this section images of the dust lane galaxies in the radio sample along with various parameters related to the dust lanes. The parameters we provide include the angle of (mis)alignment between the dust lane and the major axis of the galaxy and between the dust lane and the radio axis. The latter is sometimes ambiguous owing to the poor quality of the radio maps.
We estimate the color excess in the dust lane by comparing the color
in it with that of the surroundings. For this purpose we used a
square aperture with side 
(3 pixels) on the 
images separately to extract magnitudes along the lane and in a
neighboring region free of dust. The mean of the color excesses,
E(B-R), obtained in this
manner is then used for further calculations. We use the standard
relation from Savage and Mathis (1979) to calculate the optical
depths in :
Here, 
denotes wavelength and
and 
respectively denote the extinction and optical depth at .
We have assumed here that the dust lane obscures all stars.
Following Burstein and Heiles (1978), the column density of neutral hydrogen and the total neutral hydrogen content in the dust disk can be obtained from
where, D is the distance to the galaxy.
We assume that the dust-to-gas ratio in these galaxies is similar
to the ratio in our Galaxy,
, to obtain the dust mass.
This is a lower limit, since not all stars
are actually obscured and the actual amount is at least 1/f
larger where f;SPMlt;1 is the fraction of stars obscured.
We describe below dust related features found in the dust lane galaxies.
with a disk
having 
). The dust lane extent is
with 
and
. The dust lane makes an
angle of 
with the major axis of the galaxy and
with the radio axis as well. There is a small galaxy to the
south-east (see Figure 
) with which 0354-263 could be associated.
A possible tidal feature is seen. Owing to the uncertainty in
redshift, this object has been excluded
from subsequent calculations in this chapter.
). The size of the dust lane is 
with 
and 
.
The dust lane makes an
angle of 
with the major axis of the galaxy.
We do not have a radio map for this object.
is large).
The dust lane extent is 
and is rather diffuse.
It has
and
. In this galaxy the
radio axis is approximately along the major axis of the galaxy and
the dust lane makes an angle of 
with both.
with a
and
. In the case of this
galaxy the major axis is approximately perpendicular to the radio
axis. The dust lane makes an angle of with the radio
axis and 
with the major axis of the galaxy.
filters. There is a companion galaxy,
which was masked during the fitting.
Lack of distortion
in the outer isophotes of both galaxies suggests that it is only a
chance superposition rather than an interacting pair.
The dust lane extent is
with a and
. In this case the
dust lane in the galaxy is approximately along the galaxy major
axis while the radio axis makes an angle of with both.
) with 
and
. The dust lane is curved
and along the
major axis of the galaxy. The radio structure is not
very well determined.
[Properties of the radio galaxies with dust lanes]
Properties of the dust lane radio galaxies from our sample.
The dust mass is calculated as described in Section .
The dust lanes are, in general, not perpendicular to the radio axis.
| Object | z | size | E(B-R) |  |  |  |  |  |
 | magnitude |  | max |  | | |||
| 0354-263 | 0.30+ |  | 0.20 | 0.42 |  | -0.010 | 45 | 45 |
| 0420-263 | 0.130 |  | 0.15 | 0.32 |  | -0.010 | NA | 10 |
| 1254-268 | 0.135 |  | 0.10 | 0.21 | | -0.003 | 30 | 30 |
| 1257-253 | 0.045 |  | 0.10 | 0.21 |  | -0.005 | 30 | 60 |
| 1323-271 | 0.044 |  | 0.10 | 0.21 | | -0.003 | 30 | 00 |
| 1344-241 | 0.019 | | 0.07 | 0.21 |  | -0.005 | 00 | 00 |