  We present the results of the B, V and I photometry of eleven southern minor
mergers. The total apparent B magnitude, integrated B-V and V-I colours were
measured. We built B, V, and I equivalent profiles for each galaxy and
decomposed them into bulge and disk components when possible. From
H$\alpha$+N[II] images we have estimated the basic photometric parameters of
the HII regions, such as position, size, B-V and V-I colours, H$\alpha$+[NII]
luminosity and $EW(H\alpha+[NII])$ equivalent width. We found a linear
correlation between the luminosity ratios of the components and their ratio of
major diameters, leading to mass ratios between 0.04 $<$ $\cal M$ $_{secondary}
/ \cal M$ $_{primary}$ $<$ 0.2, suggesting indeed that our sample is formed by
minor mergers. Most of the HII regions and evolved star-forming regions of the
sample were formed between 3.6 to 13.7 Myr ago with an average of (6.3$\pm$0.7)
Myr. The HII region properties, luminosity, sizes and ages are similar in both
components. The HII regions have log(H$\alpha$+[NII]) luminosity between 38.6
and 41.7. The HII region luminosity function for the whole sample fits a power
law of index $\alpha$ = --1.33. The linear correlation between the luminosity
$\cal L$(H$\alpha$+[NII]) and the size of the HII regions has slope of
2.12$\pm$0.06. We found that the disk of the primary component is more luminous
than those of Lu's sample, while the disk of the secondary is smaller and
fainter.
