Sample of minor merger of galaxies: Optical CCD surface photometry and HII region propertie

D. L. Ferreiro; M. G. Pastoriza

doi:10.1051/0004-6361:20035894

paper

Sample of minor merger of galaxies: Optical CCD surface photometry and HII region propertie

arXiv:astro-ph/0409150 · doi:10.1051/0004-6361:20035894

Abstract

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 $α$ +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 $α$ +[NII] luminosity and $E W (H α + [N I I])$ 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 $<$ $M$ $_{seco n d a r y} / M$ $_{p r ima r y}$ $<$ 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 $α$ +[NII]) luminosity between 38.6 and 41.7. The HII region luminosity function for the whole sample fits a power law of index $α$ = --1.33. The linear correlation between the luminosity $L$ (H $α$ +[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.

arXiv comment28 pages, 19 figures, recently accepted for publication in Astronomy and Astrophysics

Sample of minor merger of galaxies: Optical CCD surface photometry and HII region propertie

Abstract

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