  We present UBVRI broad band, H$\alpha$ narrow band photometry of the star
forming complexes in the infra-red bright galaxy NGC 1084. Results of medium
resolution spectroscopy of some of the brighter complexes are also discussed.
Spectroscopic data is used to better estimate the internal reddening within the
galaxy which is found to be highly variable and to calculate metallicity which
is close to the solar value. Diagnostic diagram identifies the shocked regions
within this galaxy. The narrow band H$\alpha$ flux and its equivalent width are
used to determine the star formation rates of the complexes and the
distribution of ages. Star formation rates for a few of the complexes are found
to be as high as 0.5 $M_{\odot}$/year. The star forming complexes lie in the
age range 3 Myr to 6.5 Myr. U-B vs V-I colour-colour mixed population model
created using the Starburst99 model colours is used to estimate the ages of the
stellar populations present within these regions. Using this technique, it is
found that the star formation in NGC 1084 has taken place in a series of short
bursts over the last 40 Myr or so. It is proposed that the likely trigger for
enhanced star formation is merger with a gas rich dwarf galaxy.
