We present results from narrow-band Hα imaging and optical spectroscopy on a blue compact dwarf (BCD) Wolf-Rayet (WR) galaxy, Mrk 22. The WR emission features namely the blue and red bumps in the optical spectrum are detected. The detection of this WR features indicates that the origin of ionized gas in galaxy could be attributed to existing young massive stars. Hence, the population of hot massive stars in galaxy is also quantified using the WR bumps luminosity. The star formation rate is estimated as 0.04 ± 0.01 solar mass per year. For this region, age of the most recent starburst is found as 5.8 ± 0.7 Myr old using Hα and Hβ equivalent widths. The GMRT HI 21cm - line radio observation reveals that the most likely triggering mechanism responsible for this starburst is interaction or merger with an HI cloud. Furthermore, the physical condition and chemical abundance for various elements are derived. Subsequently, the Oxygen abundance is also estimated from electron temperature of the ionized gas.