2 The sample

The sample of 72 irregular dwarf galaxies is a compilation of Im, BCD, and late-type S galaxies fainter than M_B=-18 mag - dwarf "irregulars'' for short - used previously for an analysis of exponential-disk model parameters relating photometric, kinematic, and environmental properties (Parodi et al. 2002). The galaxies are lying in the field or in groups within the nearby 10 Mpc volume. They were imaged with 1.2-m to 1.5-m telescopes with resolutions of 0.39-0.77 arcsecs per pixel and under seeing conditions varying between 0.8 and 4.0 arcsecs. Data reduction was performed consistently by our team along the usual prescriptions. B-band galaxy image galleries can be found in Parodi et al. (2002) and the references given therein (or at the bottom of Table 2 in the present paper).

In Table 2 we list basic galaxy data as well as parametric data as deduced in the subsequent sections. The first nine columns are mostly taken over from Table 1 in Parodi et al. (2002), while the seven other columns correspond to results obtained in the present paper. The columns read as follows:
Cols. 1 and 2 give the galaxy name and the galaxy type;
Cols. 3 and 4 list the B-band absolute magnitude and - from fitting an exponential law to the observed surface brightness profile - the extrapolated central surface brightness, both corrected for galactic extinction;
Cols. 5-7 give the B-band disk scale length along the semi-major axis (in parsecs), the radius of the 25th-mag/arcsec² isophote (in parsecs), and the axis ratio of the elliptical isophote, respectively;
Col. 8 lists the rotational velocities of the galaxies as far as measured. The four entries for the southern hemisphere galaxies ESO 473-G024, IC 2038, ESO 490-G017, and ESO 059-G001 are based on HIPASS public data, treated as in Parodi et al. (2002);
Col. 9 points to the five published papers of our series with original and detailed observational and photometric data on the galaxies. Cf. the reference notes on the bottom of Table 2;
Col. 10 indicates the number of bright lumps found in residual galaxy images (Sect. 3);
Cols. 11-13 give the scale length of the radial number density distribution of the bright lumps (Sect. 4.2), the radius of the highest peak in the radial lump number distribution, and the peak radius of a possible secondary, minor peak, respectively (Sect. 4.4) (all lengths in units of scale length $R_{\rm d}$);
Cols. 14-16 list the values for the following indices: the normalized concentration index CI measured using R₂₅ as the outer aperture radius (Sect. 4.3), the reduced cluster (or correlation) dimension D (Sect. 5), and the lumpiness index $\chi$ (Sects. 3 and 6), respectively.