Herschel observations revealed omnipresent filamentary structures in Galactic star-forming clouds. Although these filaments are often identified with flowing gas that could aid the star formation, a direct implication of it might be identifying a correlation between the protostellar accretion and gas flow along the filaments. However, it is difficult to have a direct detection of accreting gas at core-scale, and thus, a solution to this problem could be finding correlation of the protostellar outflows associated with the filamentary structures. With the assumption that filaments enhance the flow of molecular gas onto protostellar accretion disks, one would ideally expect a preferred position angle of bipolar outflows with respect to the orientation of the long-axis of the filaments. I shall present a detailed study of protostellar outflows in several Galactic massive protoclusters using ALMA observations (CO, HCN and HCO+ data).
Owing to enormously high mass-loss rates (~10^-5 Msun/yr) and strong stellar winds (1000-5000 km/s), massive W-R stars have the ability to either influence their surrounding gas for further star formation or disperse the surrounding gas into the interstellar medium. We have investigated five Galactic massive star-forming regions associated with Wolf-Rayet stars for this possibility. Details of this study will be also presented.