Table 1 (click here) lists the 83 target galaxies, of which 73
belong to the complete sample. Of the other ten objects in brackets,
four of them have slightly lower infrared luminosities
than 1011.5 
and six
are fainter than our magnitude limit 
. This table presents the
infrared luminosities in unit of , magnitudes
and redshifts. All of these data were derived from the 2 Jy catalog,
except that in the case of IR 09517+6954 (M 82). We cannot use redshift as a distance indicator on account of the proximity.
For this reason, we adopted the distance value given by
Tully (1988).
These objects flagged with asterisks in Col. 1 are the sources which are also included in
the IRAS Bright Galaxy Sample 
of
Kim et al. (1995). A detailed comparison between these two
samples will be made in Paper II.
The spatial distribution of the 73 sample galaxies on the
sky is shown in Fig. 1 (click here). The dotted curve is the celestial
equator. The scarcity of objects near galactic declination
is due to the
matching Zwicky catalog (1961-1968)
which misses galaxies at low latitude.
Figure 1: The distribution of very luminous IRAS galaxies
in the sky shown in equal area projection using Galactic coordinates
Figure 2: Distribution of redshifts. The solid boxes represent our
complete samples while the dotted boxes include the other
ten galaxies
Figure 3: Distribution of infrared luminosities. The
solid and dotted boxes represent the same galaxies
as they do in Fig. 2 (click here)
Figure 2 (click here) shows the sample distribution as a function of redshift. The solid boxes represent the complete
sample, while the dotted boxes include the other ten sources. It is clear that the
redshifts concentrate in the range 0.02 to 0.04. The
median value is 0.0324 (corresponding to a recession velocity
) which is larger than
the value 
obtained by
Kim et al. (1995)
for their sample.
The infrared luminosity distribution is shown in Fig. 3 (click here). The solid and dotted
boxes correspond to the same samples as in Fig. 2 (click here).
The counts decrease rapidly as the
infrared luminosity increases. Most of the galaxies have infrared luminosities
) between 11.5 and 12.0.
| IRAS a |  | mag | z | IRAS | | mag | z |
| (1) | (2) | (3) | (4) | (1) | (2) | (3) | (4) |
| 00189+3748 | 11.572 | 15.30 | 0.0364 | 13136+6223* | 11.937 | 15.10 | 0.0311 |
| 00267+3016 | 11.966 | 14.80 | 0.0504 | 13183+3423* | 11.863 | 14.80 | 0.0230 |
| 00509+1225 | 11.772 | 14.00 | 0.0604 | 13299+1121 | 11.516 | 14.50 | 0.0317 |
| 01173+1405* | 11.868 | 14.90 | 0.0312 | 13362+4831* | 11.706 | 14.10 | 0.0275 |
| 01324+2138 | 11.629 | 15.30 | 0.0472 | 13373+0105* | 11.701 | 13.80 | 0.0225 |
| 01484+2220* | 11.851 | 13.70 | 0.0324 | 13428+5608* | 12.392 | 15.00 | 0.0373 |
| 01572+0009 | 12.665 | 15.20 | 0.1630 | 13458+1540 | 11.821 | 15.00 | 0.0570 |
| 02071+3857 | 11.546 | 13.00 | 0.0179 | 13496+0221 | 11.752 | 15.00 | 0.0328 |
| 02203+3158 | 11.837 | 14.90 | 0.0338 | 13536+1836 | 11.611 | 14.80 | 0.0497 |
| 02222+2159 | 11.652 | 14.90 | 0.0338 | 14151+2705 | 11.565 | 15.10 | 0.0365 |
| 02248+2621 | 11.519 | 14.60 | 0.0327 | 14178+4927* | 11.541 | 15.40 | 0.0256 |
| 02435+1253* | 11.501 | 15.20 | 0.0216 | 14547+2448* | 11.897 | 14.60 | 0.0339 |
| 02512+1446* | 11.780 | 14.60 | 0.0312 | 14568+4504 | 11.501 | 14.60 | 0.0357 |
| 03117+4151 | 11.562 | 14.00 | 0.0235 | 15107+0724* | 11.525 | 15.50 | 0.0131 |
| (05084+7936) | 12.170 | 15.80 | 0.0543 | 15163+4255* | 12.072 | 14.90 | 0.0402 |
| (05414+5840) | 11.505 | - | 0.0148 | 15327+2340* | 12.464 | 14.40 | 0.0182 |
| (06538+4628) | 11.490 | 13.70 | 0.0214 | 15425+4114 | 11.515 | 14.20 | 0.0317 |
| (07062+2041) | 11.559 | - | 0.0174 | 15426+4116 | 11.546 | 13.90 | 0.0319 |
| 07063+2043 | 11.570 | 12.60 | 0.0173 | 16104+5235* | 11.687 | 14.50 | 0.0294 |
| (07256+3355*) | 11.467 | 14.70 | 0.0135 | 16180+3753 | 11.592 | 14.30 | 0.0307 |
| 08354+2555* | 11.781 | 14.40 | 0.0184 | 16284+0411* | 11.582 | 14.90 | 0.0246 |
| 08507+3520 | 11.811 | 15.00 | 0.0559 | 16504+0228* | 12.028 | 14.70 | 0.0243 |
| (09047+1838) | 11.490 | 14.80 | 0.0291 | 16577+5900* | 11.582 | 14.20 | 0.0187 |
| 09126+4432* | 11.913 | 14.90 | 0.0393 | 16589+0521 | 11.637 | 15.50 | 0.0502 |
| 09168+3308 | 11.725 | 15.30 | 0.0499 | 17366+8646 | 11.544 | 14.60 | 0.0264 |
| 09320+6134* | 12.220 | 15.50 | 0.0392 | 17392+3845 | 11.554 | 15.00 | 0.0410 |
| 09333+4841* | 11.523 | 15.00 | 0.0259 | 17501+6825 | 11.829 | 15.20 | 0.0512 |
| (09517+6954) | 10.833 | 9.57 | 0.0009 | 18525+5518 | 11.683 | 15.50 | 0.0484 |
| 10203+5235 | 11.620 | 15.00 | 0.0322 | 18595+5048 | 11.501 | 15.10 | 0.0271 |
| (10311+3507) | 12.096 | - | 0.0710 | 19120+7320 | 11.624 | 15.10 | 0.0250 |
| (10565+2448*) | 12.245 | 16.00 | 0.0431 | 20550+1656* | 12.074 | 15.20 | 0.0364 |
| 11231+1456* | 11.809 | 15.40 | 0.0341 | 22388+3359* | 11.531 | 15.00 | 0.0214 |
| 11254+1126 | 11.800 | 14.80 | 0.0410 | 22501+2427 | 11.723 | 15.30 | 0.0421 |
| 11257+5850 | 12.040 | 11.80 | 0.0104 | 23007+0836* | 11.734 | 13.06 | 0.0162 |
| 11543+0124 | 11.716 | 15.20 | 0.0397 | 23024+1916* | 11.573 | 15.20 | 0.0248 |
| (12112+0305) | 12.531 | - | 0.0724 | 23135+2516* | 11.730 | 15.00 | 0.0273 |
| 12120+6838 | 12.029 | 15.40 | 0.0608 | 23254+0830* | 11.568 | 13.60 | 0.0290 |
| 12251+4026 | 11.660 | 15.00 | 0.0371 | 23488+1949* | 11.528 | 13.39 | 0.0142 |
| 12265+0219 | 12.663 | 13.07 | 0.1583 | 23488+2018* | 11.609 | 14.90 | 0.0179 |
| 12323+1549 | 11.766 | 15.20 | 0.0461 | 23532+2513 | 11.795 | 15.00 | 0.0571 |
| 12540+5708* | 12.636 | 14.10 | 0.0418 | 23594+3622 | 11.586 | 15.40 | 0.0321 |
| 12592+0436 | 11.787 | 15.50 | 0.0371 | ||||
| a The sources marked * in Col. (1) were also observed by Kim et al. (1995). | |||||||