A brief discussion is given here on some individual sources.
:
This galaxy lies in the sky close to SMC. The field is therefore crowded with
SMC foreground stars. This contamination, added to a poor seeing,
make it difficult to determine the morphology of the system.
However, a central extended object, from which we got the spectrum displayed
in Fig. 5 (click here), a tidal tail and two possible
companions seem to be associated with IRAS 00199-7426.
:
There are two galaxies in the field separated by a distance of 40
(42 kpc). Surprisingly, the
IRAS position is centered on the western object,
which is less luminous, in the optical, that the eastern disturbed spiral.
Contrary to its companion, the infrared ultraluminous galaxy seems to have a
regular spiral morphology. Since IRAS had a limited angular
resolution, varying between 1
and 5, it is not clear
whether in pairs, both galaxies are enhanced in the far infrared
(Xu & Sulentic 1991; Surace et al. 1993).
In IRAS 09111-1007, the two galaxies (which are indeed at the same distance;
the difference in velocity is only 300 km s-1)
show strong optical lines. However, compared to the eastern object, the
western one is extremely absorbed.
H
is invisible and there is a strong Na absorption line, which indicates a
high dust content. Moreover, the radio continuum source associated
with this source is stronger than the one associated with the
companion (Karoji et al. 1986). Since there is a tight correlation
between
radio and far infrared fluxes (eg.
Wunderlich et al. 1987), we can argue that
most of the far infrared
luminosity in this system comes from the western component.
:
It has two tidal tails, one prominent to the North with a condensation at its tip,
and another fainter to the South-East. Both optical and infrared images
show a single nucleus. This might be a merger in an advanced stage.
:
There is no obvious companion to this elliptical-like galaxy. Faint clumps
can be found in the outskirts of the main body. It is likely to be a
merger in a final stage.
:
The IRAS flux is concentrated on the northern spiral object of this loose
interacting pair. The galaxy is
highly disturbed. A long tail with bright condensations escapes to the North.
An arc structure is seen to the West. Its Seyfert 1 spectrum shows
strong iron FeII lines. Two line systems, separated by 
,
are seen in the 
and [OIII] line profiles. This object will be discussed
in more details in a future paper.
:
This isolated object has an eccentric nucleus, also seen in the infrared
(Murphy et al. 1996), which is an hint for
a complete merger classification.
:
It has faint tidal tails and a disturbed morphology in
the central region, with a bright nucleus surrounded by condensations
(similar to HII regions) and absorption features. In the K band however, the
dust lanes disappear and only one nucleus shows up. It's luminosity profile follows the classical r1/4 de Vaucouleurs law for ellipticals. This is a
case where an elliptical galaxy is being formed after a disk-disk
collision. Martin et al. (1989) have shown that this object is an OH megamaser.
:
This
spectacular object, also known as "the Super-Antennae''
has been discussed in details by Mirabel et al.
(1991) and Colina et al. (1991).
:
No clear nucleus can be found
in either interacting disk. Murphy et al. (1996) have shown that only the EW disk
emits in K.
:
Two diffuse tails can be seen. The nucleus is clearly elongated to the East in
the R band. After a deconvolution by a gaussian PSF, with a Maximum
Entropy method, two condensations
separated by 2.6 (4.5 kpc) show up. In the infrared, however
there is only a marginal detection at the position of the faintest source.
:
With an infrared luminosity of 
,
it is the brightest source of our sample. It appears as a disk-disk collision.
The northern disk seems to vanish in the K band.
:
This is one of the ambiguous systems in the sample. Two main galaxies are
visible, apparently separated by 41 kpc (we do not have a redshift for
the eastern object). The IRAS flux is concentrated on
the western object. None of the galaxies show clear tidal disturbances.
Faint objects
can be seen in the vicinity of IRAS 20414-1651/W.
:
discussed in details by Johansson (1991). Only one nucleus
appears in the R and K bands of this merger.
(the so-called "South America Galaxy''):
Carico et al. (1990) have shown, in the K band image, two nuclei
separated by 2 (3 kpc).
(the "Bat galaxy''):
discussed in details by Bergvall & Johansson (1985) and
Johansson & Bergvall (1988). The wings of
this object are tidal features, whereas its eyes are the nuclei of the
merging galaxies.
:
The nucleus seems to be elongated in the optical to the East. After deconvolution with a gaussian, one can infer a nuclei separation of
2.4 (4.1 kpc).
The infrared image shows an elongated nucleus, but does not confirm that
it is double.
:
Two nuclei are visible but one is at least twice as bright as the other in
the optical. In K, the ratio is 10.