It has long been speculated that Blue Compact Dwarf galaxies (BCDs) are formed through the interaction between low-mass gas-rich galaxies, but due to a lack of evidence, this possibility has rarely been explored. We study a sample of compact star-forming dwarf galaxies that are selected from a merging dwarf galaxy catalog. We present a detailed study of their spectroscopic and structural properties. We find that these BCDs looking galaxies host extended stellar shells and thus is confirmed to be a dwarf-dwarf merger. Their stellar masses range between 8 × 107 Mʘ and 2 × 109 Mʘ. Although the extended tail and shell are prominent in the deep optical images, the overall major axis light profile is well modeled with a two-component Sersic function of inner compact and extended outer radii. We calculate the inner and outer component stellar-mass ratio using the two-component modeling. We find an average of 4:1 (with a range of 10:1 to 2:1) for our sample, indicating that these galaxies might have suffered a satellite accretion which triggers the starburst in the center of the host galaxies. From the measurement of Hα equivalent width, we derived the star-formation ages of these galaxies. The derived star-formation ages of these galaxies turn out to be less than 100 Myr, suggesting the recent ignition of star-formation due to events of satellite interaction.
Key words: galaxies: evolution-galaxies: irregular-galaxies: dwarf-galaxies: starburst-galaxies: interactions.
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