  It has long been speculated that Blue Compact Dwarf galaxies (BCDs) are
formed through the interaction between low-mass gas-rich galaxies, but a few
candidates of such systems have been studied in detail. 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 are confirmed to be a dwarf-dwarf merger. Their stellar
masses range between $8\times10^7$~M$_{\sun}$ and $2\times10^9$~M$_{\sun}$.
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
S\'ersic 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 ratio of 4:1 (with a range of 10:1 to 2:1) for our sample,
indicating that the central component dominates the stellar mass with an
ongoing burst of star-formation. From the measurement of H$_\alpha$ equivalent
width, we derived the star-formation ages of these galaxies. The derived
star-formation ages of these galaxies turn out to be in the order of a few 10
Myr, suggesting the recent ignition of star-formation due to events of
satellite interaction.
