In Fig.1 (click here), the distribution of our galaxy candidates is shown. Even
at first glance, there are two obvious characteristics. First,
one notices a pronounced preponderance in numbers of galaxies at
negative galactic latitudes, from 
.
Second, there appears to be a marked connection across the galactic
plane, at 
and an extended clump of
galaxies at 
.
Figure 1:
Right: distribution of the new galaxies in galactic coordinates.
Left: the 60
flux density taken from the IRAS Sky Survey Atlas; black (white) areas
correspond to low (high) flux densities. Both parts of the figure represent
the same region.
A cross-check with the distribution of dark nebulae of
Lynds (1968) shows that the "holes'' in the distribution
(e.g. at 
and 
) for the former
location partly does, but for the latter one does not coincide
with dust clouds. The above-mentioned preponderance might be
related to the location of these (mostly nearby) obscuring clouds
preferentially above the plane there. Anyway, the asymmetrical distribution
in the region 
is probably
due to the existence of the galactic warp, evident as the
bending of the dust layer (see also Freudenreich et al. 1994).
In this context we found that the 60 (Fig.1 (click here)) or 100 IRAS sky
flux densities that are an approximate measure of the total extinction in front
of the galaxies (see Paper II), accord roughly with their
distribution. In other words, the distribution appears to reflect
the distribution of the galactic dust, and galaxy concentrations are rather
holes or transparent locations in the dust layer than real clusters
of galaxies. In the region 
the distribution of the
galaxies as well as the 60 IRAS flux densities appear to be symmetrical
with respect to the galactic equator. The reason for this can be attributed to
the crossing of the dustlayer with the galactic equator.
The excess of galaxies at about 
was first
noted by Weinberger (1980) who called it a "striking
conglomerate of galaxies''. The bridge-like appearance in Fig. 1 (click here), across
the galactic plane, however brings to mind the frequently raised
question whether or not the main ridge of the Perseus-Pisces
supercluster crosses the ZOA and connects to structures in the
norther galactic hemisphere including the 3C129 cluster
at and 
(Hauschildt
1987) and cluster Abell569 at 
and 
(Focardi et al. 1984; Chamaraux et al.
1990). According to new and extensive 21 cm measurements this
problem appears to be settled: Lu & Freudling (1995) report
that it is still possible that 3C129 is connected
to the main ridge of the PP supercluster, but a connection to Abell569
can probably be ruled out. For the bridge in Fig.1 (click here) this result
consequently is not entirely conclusive: again it calls for
further measurements, since Lu & Freudlings's conclusion obviously
does not exclude at least a partial crossing, up to 
.
In Table 1 (click here) our list of 1067 optical galaxy candidates is presented. The whole compilation is available from the SIMBAD database. The columns have the same meaning as in Paper III. Note that in this table the letters E and O correspond to the POSSI-E (red-sensitive) and POSSI-O (blue-sensitive) prints, respectively. Maximum and minimum diameters were determined and are presented in ar-
cmin. In addition, mean average bulge (b)
diameters are given.
All diameters listed
have an accuracy (of measurement) of 
mm,
but are presented in hundredths of arcmin to avoid biases that
would occur in the course
of rounding.
A colon means that a galactic nature of the object cannot be excluded.
An asterisk was used when more than one optical galaxy fell within the
boundaries of one IRAS point source error ellipse.
| ZOAG |  (B1950.0) |
 (B1950.0) |
(J2000.0) |
(J2000.0) | POSS | x(mm) | y(mm) |
E |
 |
O |
 | cross id. | ||
| G130.00+3.61 | 01 56 40 | +65 17.4 | 02 00 26 | +65 31.9 | 878 | 142.9 | 112.9 | 0.22 | 0.11 | 0.22 | 0.06 | |||
| G130.00+3.60 | 01 56 38 | +65 16.7 | 02 00 24 | +65 31.2 | 878 | 143.1 | 112.3 | 0.17 | 0.06 | |||||
| G130.02+3.63 : | 01 56 56 | +65 18.1 | 02 00 42 | +65 32.6 | 878 | 141.5 | 113.6 | 0.11 | 0.06 | |||||
| G130.09-3.97 | 01 42 34 | +57 53.4 | 01 45 55 | +58 08.4 | 1240 | 113.7 | 33.3 | 0.11 | 0.22 | |||||
| G130.11-4.34 | 01 42 10 | +57 31.5 | 01 45 30 | +57 46.5 | 1240 | 116.0 | 13.8 | 0.22 | 0.11 | 0.06 | 0.11 | 0.06 | ||
| G130.24-4.18 | 01 43 21 | +57 39.1 | 01 46 42 | +57 54.1 | 1240 | 107.7 | 20.8 | 0.34 | 0.22 | 0.17 | ||||
| G130.29+1.65 | 01 54 41 | +63 19.4 | 01 58 20 | +63 34.0 | 878 | 152.1 | 7.6 | 0.06 | 0.06 | WEIN171) | ||||
| G130.46+4.94 | 02 04 29 | +66 26.4 | 02 08 23 | +66 40.6 | 878 | 102.9 | 176.1 | 0.11 | ||||||
| G130.53-4.92 | 01 44 16 | +56 52.3 | 01 47 36 | +57 07.2 | 1245 | 288.3 | 307.0 | 0.34 | 0.22 | 0.34 | 0.22 | CGCG559-02 | ||
| G130.53-2.17 | 01 48 53 | +59 33.5 | 01 52 20 | +59 48.3 | 1240 | 73.9 | 124.3 | 0.22 | 0.11 | 0.22 | 0.11 | |||
| G130.65-4.10 | 01 46 27 | +57 38.9 | 01 49 49 | +57 53.8 | 1240 | 85.5 | 21.6 | 0.11 | 0.11 | |||||
| G130.72-4.19 | 01 46 50 | +57 32.6 | 01 50 12 | +57 47.5 | 1240 | 82.5 | 16.0 | 0.11 | 0.11 | |||||
| G130.76-3.62 | 01 48 04 | +58 05.6 | 01 51 27 | +58 20.4 | 1240 | 75.3 | 45.8 | 0.22 | 0.17 | 0.22 | 0.17 | |||
| G130.77-2.84 | 01 49 32 | +58 51.0 | 01 52 58 | +59 05.8 | 1240 | 67.3 | 86.8 | 0.22 | 0.06 | 0.11 | 0.06 | |||
| G130.78-2.67 : | 01 49 53 | +59 00.8 | 01 53 19 | +59 15.6 | 1240 | 65.4 | 95.6 | 0.17 | 0.06 | 0.11 | 0.06 | |||
| G130.81+4.49 : | 02 06 32 | +65 54.8 | 02 10 26 | +66 08.9 | 878 | 90.1 | 148.6 | 0.22 | 0.11 | |||||
| G130.86-4.00 | 01 48 11 | +57 41.7 | 01 51 34 | +57 56.5 | 1240 | 73.3 | 24.7 | 0.11 | 0.06 | |||||
| G130.92-4.09 | 01 48 25 | +57 35.8 | 01 51 48 | +57 50.6 | 1240 | 71.3 | 19.5 | 0.11 | 0.06 | 0.22 | 0.06 | |||
| G131.04-4.20 : | 01 49 09 | +57 27.6 | 01 52 32 | +57 42.4 | 1240 | 65.7 | 12.4 | 0.11 | 0.11 | |||||
| G131.13+3.11 | 02 05 35 | +64 30.1 | 02 09 23 | +64 44.3 | 878 | 90.5 | 73.1 | 0.11 | 0.11 | |||||
| G131.23-2.27 | 01 54 05 | +59 17.6 | 01 57 33 | +59 32.2 | 1240 | 37.7 | 112.4 | 0.67 | 0.17 | 0.11 | 0.22 | |||
| G131.24-3.49 : | 01 51 52 | +58 06.0 | 01 55 17 | +58 20.7 | 1240 | 48.5 | 47.8 | 0.11 | 0.06 | |||||
| G131.30-2.27 : | 01 54 38 | +59 16.2 | 01 58 07 | +59 30.8 | 1240 | 33.9 | 111.5 | 0.11 | ||||||
| G131.30-3.45 | 01 52 21 | +58 07.8 | 01 55 46 | +58 22.5 | 1240 | 45.2 | 49.6 | 0.22 | 0.06 | |||||
| G131.32+4.61 | 02 11 36 | +65 52.1 | 02 15 32 | +66 06.0 | 878 | 62.3 | 148.4 | 0.45 | 0.22 | 0.34 | 0.13 | IRAS02115+6552 | ||
| G131.42-4.18 | 01 51 54 | +57 23.4 | 01 55 18 | +57 38.1 | 1245 | 231.6 | 332.5 | 0.56 | 0.28 | 0.45 | 0.11 | |||
| G131.48-3.04 | 01 54 28 | +58 28.8 | 01 57 55 | +58 43.4 | 1240 | 31.7 | 69.3 | 0.17 | 0.11 | 0.22 | 0.11 | |||
| G131.70-3.20 | 01 55 46 | +58 16.0 | 01 59 13 | +58 30.5 | 1240 | 21.6 | 58.7 | 0.11 | 0.11 | |||||
| G131.72+3.49 : | 02 11 55 | +64 40.7 | 02 15 47 | +64 54.6 | 878 | 55.0 | 85.2 | 0.28 | 0.17 | 0.10 | ||||
| G131.81-4.28 | 01 54 30 | +57 11.6 | 01 57 54 | +57 26.2 | 1245 | 212.8 | 321.5 | 0.67 | 0.56 | 0.34 | 0.45 | 0.22 | 5Zw1532) | |
| G131.90-4.33 | 01 55 04 | +57 07.5 | 01 58 28 | +57 22.1 | 1245 | 209.0 | 317.8 | 0.17 | 0.11 | 0.22 | 0.11 | |||
| G131.91-4.09 | 01 55 36 | +57 21.5 | 01 59 01 | +57 36.1 | 1245 | 204.9 | 330.3 | 0.17 | 0.06 | 0.11 | 0.06 | |||
| G131.92-4.22 | 01 55 24 | +57 13.7 | 01 58 49 | +57 28.3 | 1245 | 206.5 | 323.4 | 0.11 | 0.09 | |||||
| G131.92-3.09 | 01 57 34 | +58 19.1 | 02 01 02 | +58 33.6 | 1240 | 9.3 | 62.4 | 0.17 | 0.06 | 0.11 | ||||
| G131.96-2.23 | 01 59 38 | +59 08.2 | 02 03 08 | +59 22.6 | 597 | 307.4 | 110.4 | 0.11 | ||||||
| G132.00+1.86 | 02 09 42 | +63 02.8 | 02 13 27 | +63 16.8 | 597 | 230.8 | 315.4 | 0.22 | 0.11 | |||||
| G132.01-4.18 | 01 56 08 | +57 14.6 | 01 59 33 | +57 29.1 | 1245 | 201.2 | 324.1 | 0.17 | 0.11 | 0.03 | ||||
| G132.13-4.65 | 01 56 05 | +56 45.6 | 01 59 29 | +57 00.1 | 1245 | 201.8 | 298.1 | 0.11 | 0.11 | |||||
| G132.14-4.75 | 01 55 58 | +56 39.9 | 01 59 22 | +56 54.4 | 1245 | 202.7 | 293.1 | 0.22 | 0.11 | 0.09 | ||||
| G132.18-3.99 | 01 57 41 | +57 23.2 | 02 01 07 | +57 37.7 | 1245 | 189.9 | 331.6 | 0.11 | ||||||
| G132.19+3.50 | 02 16 02 | +64 32.3 | 02 19 56 | +64 46.1 | 1241 | 333.6 | 79.6 | 0.22 | ||||||
| G132.31-5.00 | 01 56 39 | +56 22.8 | 02 00 03 | +56 37.3 | 1245 | 197.8 | 277.8 | 0.11 | 0.22 | |||||
| G132.37+3.93 | 02 18 59 | +64 53.2 | 02 22 55 | +65 06.8 | 1241 | 314.7 | 96.3 | 0.11 | 0.11 | |||||
| G132.41-4.42 : | 01 58 31 | +56 54.7 | 02 01 56 | +57 09.2 | 1245 | 183.9 | 306.2 | 0.11 | 0.11 | |||||
| G132.45-3.38 | 02 00 50 | +57 54.1 | 02 04 18 | +58 08.5 | 597 | 303.7 | 43.7 | 0.39 | 0.22 | MCG+10-04-01 | ||||
| G132.54+3.85 | 02 20 11 | +64 44.9 | 02 24 07 | +64 58.5 | 878 | 8.3 | 93.8 | 0.11 | 0.11 | 0.09 | ||||
| G132.59-3.20 | 02 02 14 | +58 01.9 | 02 05 43 | +58 16.2 | 597 | 293.5 | 50.1 | 0.28 | 0.06 | 0.03 | 0.11 | |||
| G132.65-4.83 | 01 59 24 | +56 26.8 | 02 02 49 | +56 41.2 | 1245 | 177.5 | 281.3 | 0.34 | 0.11 | 0.22 | 0.11 | |||
| G132.67-3.23 | 02 02 45 | +57 59.2 | 02 06 14 | +58 13.5 | 597 | 289.9 | 47.5 | 0.17 | 0.11 | 0.17 | 0.11 | |||
| G132.68-4.84 : | 01 59 33 | +56 26.2 | 02 02 58 | +56 40.6 | 1245 | 176.3 | 280.7 | 0.11 | 0.06 | |||||
| G132.76+4.13 | 02 23 06 | +64 56.3 | 02 27 05 | +65 09.8 | 1241 | 291.3 | 96.9 | 0.34 | ||||||
| G132.90+4.17 | 02 24 28 | +64 55.6 | 02 28 27 | +65 09.0 | 1241 | 283.5 | 95.6 | 0.22 | 0.17 | 0.17 | 0.11 | 0.06 | ||
| G133.32-4.05 : | 02 05 39 | +57 00.3 | 02 09 07 | +57 14.5 | 1245 | 132.0 | 311.7 | 0.22 | ||||||
| G133.47-4.61 | 02 05 31 | +56 26.0 | 02 08 58 | +56 40.2 | 1245 | 132.3 | 281.0 | 0.12 | 0.11 | |||||
| G133.47-4.40 : | 02 05 54 | +56 38.2 | 02 09 22 | +56 52.4 | 1245 | 129.6 | 292.0 | 0.22 | 0.06 | 0.22 | 0.06 | |||
| G133.48+2.75 : | 02 24 45 | +63 23.2 | 02 28 39 | +63 36.6 | 1241 | 288.3 | 13.4 | 0.11 | ||||||
| G133.61-4.68 | 02 06 16 | +56 19.4 | 02 09 43 | +56 33.6 | 1245 | 126.5 | 275.3 | 0.28 | 0.11 | 0.17 | 0.06 | |||
| G133.63-3.61 | 02 08 48 | +57 20.1 | 02 12 18 | +57 34.2 | 1245 | 109.6 | 330.1 | 0.67 | 0.45 | 0.06 | 0.90 | 0.45 | 0.06 | |
| G133.68-4.93 | 02 06 13 | +56 04.0 | 02 09 40 | +56 18.2 | 1245 | 126.5 | 261.6 | 0.17 | 0.03 | 0.17 | ||||
| G133.83-4.07 : | 02 09 10 | +56 50.0 | 02 12 39 | +57 04.0 | 1245 | 106.0 | 303.3 | 0.11 | 0.11 | |||||
| G133.83+3.40 | 02 29 47 | +63 51.8 | 02 33 45 | +64 05.0 | 1241 | 256.7 | 36.8 | 0.56 | 0.22 | 0.34 | 0.17 | IRAS02297+6351 | ||
| G133.84-4.08 | 02 09 12 | +56 49.8 | 02 12 41 | +57 03.8 | 1245 | 105.7 | 303.1 | 0.10 | ||||||
| G133.87-4.84 | 02 07 43 | +56 05.8 | 02 11 10 | +56 19.9 | 1245 | 115.5 | 263.5 | 0.22 | 0.11 | 0.22 | 0.11 | |||
| G134.02+4.67 | 02 35 59 | +64 57.5 | 02 40 04 | +65 10.4 | 1241 | 218.3 | 93.8 | 0.34 | 0.13 | IRAS02359+6457 | ||||
| G134.05-4.45 : | 02 09 50 | +56 24.8 | 02 13 19 | +56 38.8 | 1245 | 100.3 | 281.0 | 0.11 | 0.07 | 0.22 | 0.11 | |||
| G134.15-1.82 | 02 16 48 | +58 52.2 | 02 20 25 | +59 05.9 | 597 | 189.9 | 91.2 | 0.17 | 0.06 | |||||
| G134.19-4.39 | 02 10 54 | +56 25.3 | 02 14 23 | +56 39.3 | 1245 | 92.4 | 281.7 | 0.22 | 0.06 | 0.22 | 0.11 | |||
| G134.22+4.06 | 02 35 29 | +64 19.4 | 02 39 31 | +64 32.3 | 1241 | 222.3 | 59.9 | 0.17 | 0.11 | IRAS02354+6418* | ||||
| G134.22+4.05 | 02 35 25 | +64 18.5 | 02 39 27 | +64 31.4 | 1241 | 222.7 | 59.1 | 0.45 | 0.11 | 0.34 | 0.11 | IRAS02354+6418* | ||
| G134.69+4.71 : | 02 41 53 | +64 43.3 | 02 46 00 | +64 55.9 | 1241 | 185.1 | 80.4 | 0.22 | 0.06 | |||||
| G134.70+4.70 | 02 41 56 | +64 42.6 | 02 46 03 | +64 55.2 | 1241 | 184.7 | 79.8 | 0.34 | 0.17 | 0.11 | 0.22 | 0.11 | 0.11 | |
| G134.81-4.07 | 02 15 54 | +56 31.8 | 02 19 25 | +56 45.6 | 1245 | 55.8 | 289.4 | 0.17 | 0.17 | IRAS02159+5631 | ||||
| G135.01-4.27 | 02 16 46 | +56 16.6 | 02 20 17 | +56 30.3 | 1245 | 48.6 | 276.2 | 0.22 | 0.11 | 0.17 | 0.11 | |||
| G135.06-4.71 | 02 16 06 | +55 50.8 | 02 19 36 | +56 04.6 | 1617 | 342.0 | 260.0 | 0.17 | 0.17 | |||||
| G135.13-4.41 | 02 17 17 | +56 06.0 | 02 20 48 | +56 19.7 | 1245 | 44.1 | 267.0 | 0.17 | 0.06 | |||||
| G135.34-4.08 | 02 19 28 | +56 20.4 | 02 23 00 | +56 34.0 | 1245 | 28.8 | 281.0 | 0.17 | 0.11 | |||||
| G135.40-4.76 : | 02 18 13 | +55 41.0 | 02 21 43 | +55 54.7 | 1245 | 35.7 | 245.3 | 0.22 | 0.06 | 0.06 | 0.11 | 0.06 | ||
| G135.61-4.21 | 02 20 59 | +56 07.7 | 02 24 31 | +56 21.3 | 1617 | 304.4 | 272.2 | 0.17 | 0.11 | 0.06 | 0.17 | 0.11 | 0.06 | |
| G135.63-4.27 | 02 20 58 | +56 03.7 | 02 24 30 | +56 17.3 | 1617 | 304.7 | 268.7 | 0.11 | 0.06 | |||||
| G135.66-3.61 | 02 22 50 | +56 40.0 | 02 26 24 | +56 53.5 | 1617 | 288.9 | 300.2 | 0.11 | 0.22 | |||||
| G135.70-3.79 | 02 22 38 | +56 29.6 | 02 26 11 | +56 43.1 | 1245 | 6.0 | 291.1 | 0.11 | 0.06 | 0.17 | ||||
| G135.71+1.75 | 02 39 10 | +61 36.4 | 02 43 04 | +61 49.1 | 597 | 46.3 | 242.1 | 0.34 | 0.11 | 0.22 | ||||
| G135.73-4.83 | 02 20 16 | +55 30.0 | 02 23 46 | +55 43.6 | 1617 | 312.0 | 239.1 | 0.17 | 0.17 | |||||
| G135.74-4.83 | 02 20 16 | +55 29.9 | 02 23 46 | +55 43.5 | 1245 | 19.5 | 236.5 | 0.22 | 0.11 | 0.22 | 0.11 | |||
| G135.74-4.53 | 02 21 03 | +55 47.1 | 02 24 34 | +56 00.7 | 1245 | 14.7 | 252.3 | 1.12 | 0.90 | |||||
In our previous papers we found that only a few percent of the optical galaxies turned out to have counterparts in the IRAS Point Source Catalogue. This holds true also for the galaxy sample presented in this paper. Since the IRAS two-colour distribution shows the same pattern as already shown and dicussed e.g. in Paper II, we will not repeat it here. The same applies for the presentation of the size distribution function that indicates a complete size limited sample down to a certain diameter limit (0.4arcmin, see Fig. 6 in Paper II).
Acknowledgements
We would like to thank W. Jais for his help in the data acquisition. This work was supported by the "Fonds zur Förderung der wissenschaftlichen Forschung'', project no. P8325-PHY and by the "Jubiläumsfonds der Österreichischen Nationalbank'', project No. 4713 (computer facilities).
, 