Understanding star formation activity in Galactic H II regions

Study of Galactic H II regions is one of the vital tools in understanding the effect
of high-mass star(s) (> 8 solar masses). Copious amount of UV photons from such stars can ionize the neighbouring ISM, injecting large energy and momentum, which leads to a host of features.  Such regions can be used as test-beds for triggered star formation theories such as radiation driven implosion and collect-and-collapse model. Tangentially, it can also be tested if such triggering processes can lead to the formation of second generation high-mass stars. The sheer complexity of an H II region makes multi-wavelength study an imperative. Observations at various wavelengths - like optical, infrared, sub-millimeter, and radio etc - are required to discern various components and morphological features of a region. We have carried out a multi-wavelength analysis of the Galactic H II regions Sh2-297 (in Canis Major OB1 complex) and W40 (in Serpens) to decipher the star formation processes going on. We present the results of the same in this talk.