3 The Catalogue

The Catalogue is presented in Table 3 through Table 6. Tables 3 and 4 present the spectroscopic parameters of all the galaxies for which a reliable internal extinction correction was done, and which account for the main body of the Catalogue. The data are arranged in Table 3 as follows:

• Column 1: The galaxy name according to Popescu et al. (1996, 1998).
• Column 2: The absolute blue magnitudes (M_B) as listed in Vennik et al. (1999).
• Column 3: The heliocentric redshift.
• Column 4: The absorption coefficient c(H${\beta }$).
• Columns 5, 6, 7, 8: The equivalent widths (W) of the H${\beta }$, [OIII]${\lambda}$5007, H$\alpha$ and [SII] ${\lambda}{\lambda}$6717, 6731 emission lines in Å.
• Column 9: The observed H${\beta }$ fluxes in erg ${\rm s}^{-1}~{\rm cm}^{-2}$, corrected for absorption.
• Column 10: Seeing corrected approximate angular size of the star-forming regions $r_{{\rm HII}}$, as measured in the B band by Vennik et al. (2000).
• Column 11: The morphological type.

Table 4 contains the corrected line ratios (normalised to H ${\beta}=100$) of the emission lines detected in the spectra of the galaxies listed in Table 3. The header of the table contains the identification of the emission line while the line below gives the corresponding restframe wavelength. The [SII] ${\lambda}{\lambda}$6724, 6731 and the [OII] ${\lambda}{\lambda}$7320, 7330 are not deblended, and therefore the line ratios refer to their blend.

Table 5 lists the galaxies for which it was not possible to deblend H$\alpha$ from [NII] ${\lambda}{\lambda}$6563, 6584, and therefore the line ratios were not corrected for internal extinction. The line ratio of H$\alpha$ corresponds to the blend with the [NII] lines. Finally, Table 6 lists those galaxies for which the H${\beta }$ emission line was too noisy to allow an accurate determination of the internal extinction, and again only the uncorrected line ratios are listed. Here, the line ratios in Col. 5 through 8 are given in units of H$\alpha$ = 100. In 8 cases it was possible to disentangle the contribution of different HII regions in the galaxy. Then the spectrum of each region was extracted separately and the fluxes measured for each individual region. In Tables 3-6 only the line ratios corresponding to the brightest HII region are given, but the H${\beta }$ fluxes are the total fluxes for the galaxy, summed over all the HII regions. In Table 7 we list the 8 galaxies with detected HII regions together with their observed H${\beta }$ fluxes. These fluxes are not corrected for absorption. The HII regions are given in order of their location along the slit, from South to North.