The Centaurus Cluster Catalogue CCC is available in electronic form at the CDS via anonymous ftp 130.79.128.5. It contains all 296 galaxies detected in the survey area and classified with a membership probability of 50% or more. For each galaxy we give a set of derived fundamental parameters. The data are organized as follows:
Column (1). Centaurus Cluster Catalogue number.
Columns (2)+(3). Right ascension and declination (1950.0). To determine the equatorial coordinates of the galaxies we drew on the star positions of the Hubble Space Telescope Guide Star Catalogue (Russel et al. 1990). For each of the 16 digitized images a well distributed sample was selected of at least 15 guide stars. Their coordinates define a reference system for the specific image and were used to convert the X-Y coordinates of the galaxies into equatorial coordinates. As an internal accuracy check we further selected on each image a second sample of 10 other guide stars. The rectangular coordinates of these stars were determined and transformed to equatorial coordinates in a similar way as those of the galaxies. The deviations of our achieved coordinates from their GSC coordinates gave the mean position error. For all 16 images of the Centaurus region this value is less than 1arcsec.
Column (4). Morphological type. The galaxy classification follows
primary the precepts of Sandage (1961) and Sandage & Binggeli (1984)
in the case of the giant galaxies and the dwarfs, respectively.
The main giant classes are: E, S0, Sa, Sb, Sc, Sd, and Sm
with intermediate classes E/S0, S0/a, Sab, etc. Barred lenticulars or spirals
are indicated as SB. Following Hubble, E and S0 galaxies are classified
according to their flattening. Thereby, the minor-to-major axis ratio b/a
of a galaxy is coded as Ex or S0(x) where 
. Dust features
in a S0 are noted by a subindex 1, 2 or 3 according to their strength
(Sandage
1961). The dwarf classes are: Im, BCD, dE, and dS0. Depending on the presence
or absence of a central nucleus, a dE or dS0 has been added by a "N".
If the uncertainty in the classification of a particular galaxy is larger
than within a subtype it was marked by a symbol.
Errors within the same Hubble type are indicated by ":" or
by "?" in the case of an even larger uncertainty.
Column (5). Cluster membership probability. 1 = definite member (100%), 2 = likely member (75%), 3 = possible member (50%).
Column (6). Total apparent blue magnitude 
. The magnitudes are not
corrected for galactic absorption into the direction of the Centaurus cluster which
is still not very well known. Published values are in the range between 
(Sandage 1973) and 0.92 (Bothun et al. 1989). A good compromise seems to be 0.42
based on HI column density observations (Burstein & Heiles 1982, 1984).
Column (7). Quality of the derived growth curve and
surface-brightness profile. 1 = the profile is not disturbed by a central
saturation effect, nor was a smoothing process necessary due to a noisy
background, 2 = a weak saturation correction was applied (effect 
in 
) or the curve was weakly smoothed. 3 = a substantial saturation
correction (effect 
in 
) or smoothing was needed. 4 =
growth
curve was reliable only to determine the total apparent magnitude 
.
Column (8). Mean effective surface brightness 
in Barcsec
.
Column (9). Logarithm of the mean effective radius 
(radius containing half of total light) in arcsec.
Column (10). Central exponential surface brightness 
in
Barcsec
.
Column (11). Logarithm of exponential scale length 
in
arcsec.
Column (12). Exponent of the generalized exponential profile (shape parameter).
Column (13). Heliocentric radial velocity in 
. The
indicated integer represents three different references: 1 =
Dickens et
al. (1986), 2 = Lucey & Carter (1988), 3 = Stein (1994).
Column (14). Various names by which each galaxy is known. The letters indicate the following 4 catalogues: B (Bothun et al. 1989), D (Dressler 1980), DCL (Dickens et al. 1986), 6 digit number (Lauberts 1982). The references for NGC galaxies are given in Table5 (click here).
Table 5: Finding list of NGC galaxies
Comment: The two galaxies CCC88 and CCC212 were strongly disturbed by
bright stars in their very near neighbourhood. No satisfactory reduction of
these images was possible and the 
-magnitudes were estimated by
eye. Other structure parameters have not been derived.