  My thesis work aims to study the inter-relation between various physical and
chemical conditions in a wide range of astrophysical environments. Our studied
regions range from the super-hot regions (i.e., nebular, photon-dominated, or
photodissociation regions, diffuse area, through which the lights of the
background stars can reach us) to the super-cold regions (i.e., dense molecular
clouds, proto-planetary disks, etc. where interstellar dust particles absorb
all background visible and ultra-violet lights). The chemical complexity of the
interstellar cloud gradually evolves due to the evolution in physical
conditions. The dense molecular clouds are the birth sites of star-formation,
where a wide variety of complex organic molecules are observed. Dust particles
play an essential role in the formation of these complex organic molecules.
During the warm-up stage of a star-forming region, the molecules formed during
the cold phase start to return to the gas phase by various thermal and
non-thermal evaporation processes. These complex molecules again freeze out to
the outer part of the proto-planetary disk during the further evolved stage
according to their condensation temperature and form the so-called snow-lines.
The binding energies of these molecules with the prevailing dust particles play
a crucial role in determining the structural information of this disk. Thus the
binding energy of the molecules is vital to understand several critical aspects
of the star and planet formation processes. In this thesis, I will discuss the
chemical complexity obtained in a wide range of the star-forming region and
whether this chemical complexity lead to biomolecules in space.
