2. Observations

As before, spectroscopic observations of the more widespread brighter () galaxies, identified in our survey, have been carried out with the 1.9 m Radcliffe reflector and UNIT Spectrograph at the South African Astronomical Observatory during four weeks in 1993 - 1995, and are reported in Sect. 2 below. We have also continued to complement these observations by programmes using the MEFOS (multi-fibre) spectrograph system (Felenbok et al. 1997) on the 3.6 m telescope at the European Southern Observatory (for fainter distant galaxies), and using the Parkes radio telescope (to cope with nearby galaxies of low optical brightness). The outcome of these complementary programmes will be presented separately.

The observations at SAAO were carried out over with a resolution of per pixel. Integration times typically range from 500 to 2500 seconds. The procedures used for observations, and the reductions carried out thereafter at the University of Cape Town, are the same as described in Paper I.

The entries in Table 1 are as follows:

Columns 1 and 2:

Identification of the galaxy as given in WKK97 and Lauberts identification (Lauberts 1982).

Columns 3 and 4:

Right Ascension and Declination (1950.0). The positions were measured with the Optronics machine at the ESO in Garching and have an accuracy of about 1 arcsec.

Columns 5 and 6:

Galactic longitude and latitude b.

Column 7:

Large and small diameters (in arcsec). The diameters are measured approximately to the isophote of 24.5 mag and have a scatter of .

Column 8:

Apparent magnitude . The magnitudes are estimates from the film copies of the SRC IIIaJ Survey based on the above given diameters and an estimate of the average surface brightness of the galaxy. The magnitudes and diameters in the Crux region are estimated by PAW but show no significant deviation from the magnitude and diameter estimates in the Hydra-Antlia region as determined by RCKK (Paper I and Table 2). A more detailed discussion on this subject will follow in WKK97.

Column 9:

Morphological type. The morphological types are coded similarly to the precepts of the Second Reference Catalogue (de Vaucouleurs et al. 1976). Due to the varying foreground extinction a homogenous and detailed type classification could not always be accomplished and some codes were added: In the first column F for E/S0 was added to the normal designations of E, L, S and I. In the fourth column the subtypes E, M and L are introduced next to the general subtypes 0 to 9. They stand for early spiral (), middle spiral () and late spiral or irregular (). The cruder subtypes are a direct indication of the fewer details visible in the obscured galaxy image. The questionmark at the end marks uncertainty of the main type, the colon uncertainty in the subtype.

Columns 10 and 11:

Heliocentric velocity (cz) and error as derived from the absorption features. The errors may appear large as they are estimated external errors, and not internal errors (see Paper I). The square brackets indicate a tentative redshift.

Columns 12 and 13:

Heliocentric velocity and error measured from the emission lines (identified in Col. 14) when present. The square brackets indicate a tentative redshift.

Column 14:

Identified emission lines: a

1 2 3 4 5 6 7

3727 4340 4861 4959 5007 6563 6584

A colon indicates the identification is tentative.

Column 15:

Code for additional remarks:
1) WKK 150: The redshift measured at the SAAO for this galaxy is in disagreement with the value quoted in the literature ( km s^-1, Fisher et al. 1995). It might be due to an identification error; a neighbouring galaxy (WKK 158) was found to be in good agreement with the value quoted in the literature.
2) The redshifts for these galaxies are tentative only, but confirmed by independent redshifts from the literature.
Sy2) These four galaxies have been classified as Seyfert 2.
PN) WKK P8: This object was classified as a possible PN, but was not listed in PNe list of Acker (1992). It has now been confirmed as a PN.
Gal) Identification as galaxy questionable, spectra indicates a galactic origin.
*) Redshifts are also available in the literature.

Table 2 represents an addendum to our Paper I, giving further redshift measurements for galaxies in the Hydra-Antlia region. The format is the same as for Table 1 and the entries in Table 2 are as in Table 1 with the exception of:

Column 1:

Identification of the galaxy as given in Kraan-Korteweg (1997) for galaxies with the prefix KK, or from Salem & Kraan-Korteweg (1997) for galaxies with the prefix SKK.

Column 8:

Apparent magnitude as determined by RCKK. These values are derived similar to the ones quoted in Paper I.

Column 15:

Code for additional remarks:
3) KK1196: The redshift measured at the SAAO for this galaxy is in slight disagreement with the value quoted in the literature (v = 2411 km s^-1, Huchtmeier & Richter 1989).
4) : The redshift measured at the SAAO for this galaxy is in slight disagreement with the value quoted in the literature (v = 6350 km s^-1, Visvanathan & v.d. Bergh 1992).
#) These galaxies are not in our search area, but do lie in the "Zone of Avoidance''. The diameters and type are from Lauberts (1982).

Special cases:

In the course of this survey we have given special attention to a number of objects that, based on their optical appearance, might be Planetary Nebulae (PNe). In the Crux region there a four such objects and these observations are described elsewhere (Kraan-Korteweg et al. 1996b): Two of the four PNe candidates were too faint to be detected, one was confirmed as being a PN (PNG 299.5+02.5) and one object was classified as a new PN (PNG 298.3+06.7).

Table 3 lists galaxies for which the spectra has too poor a signal-to-noise ratio for a redshift to be extracted. For one galaxy (WKK 647) the spectrum was dominated by a superimposed foreground star and no reliable redshift could be extracted.

Table 4 lists the galaxies with their optical properties as determined in our Crux survey, for which redshifts have already been published in the literature. Although now reobserved by us, these galaxies clearly would have been included in our observations, since they meet our selection criteria. Columns 1-9 are the same as in Table 1. Columns 10 and 11 list the heliocentric velocities and errors (if given). The velocity in Col. 10 has been adopted from the source identified in Col. 12, where the number corresponds to:

1. Dressler (1991), The supergalactic plane redshift survey.
2. Strauss et al. (1992), A redshift survey of IRAS galaxies.
3. Visvanathan & v.d. Bergh (1992), Luminous spiral galaxies in the direction of the Great Attractor.
4. Fairall (1983), Spectroscopic survey of southern compact and bright-nucleus galaxies.
5. Fisher et al. (1995), The IRAS 1.2 Jy Survey.
6. Fairall (1996), The Southern Redshift Catalogue.

2.1. Comparison to other measurements

Although the galaxies we observed were initially selected on the basis of having no published redshifts, more recent publications have provided redshifts from other investigators for 20 of the galaxies in Table 1 and Table 2. This overlap, however, allows a suitable comparison between our sample and others. We find

which shows no significant systematic error, and agrees well within our average standard deviation.

Similarly, we have allowed a small overlap between the SAAO galaxies and our complementary programmes using Mefos and Parkes radio observations, for which we find

The comparison with the MEFOS and Parkes data is based on 5 and 12 galaxies respectively. Again, the agreement is acceptable with our standard deviation; the latter in any case probably reflects low surface-brightness galaxies, for which our errors are at their largest values.