We have performed a multi-wavelength analysis of a mid-infrared ( MIR ) bubble N37 and its surrounding environment .
The selected 15 ^ { \prime } \times 15 ^ { \prime } area around the bubble contains two molecular clouds ( N37 cloud ; V _ { lsr } \sim 37–43 km s ^ { -1 } , and C25.29+0.31 ; V _ { lsr } \sim 43–48 km s ^ { -1 } ) along the line of sight .
A total of seven OB stars are identified towards the bubble N37 using photometric criteria , and two of them are spectroscopically confirmed as O9V and B0V stars .
Spectro-photometric distances of these two sources confirm their physical association with the bubble .
The O9V star is appeared to be the primary ionizing source of the region , which is also in agreement with the desired Lyman continuum flux analysis estimated from the 20 cm data .
The presence of the expanding H ii region is revealed in the N37 cloud which could be responsible for the MIR bubble .
Using the ^ { 13 } CO line data and photometric data , several cold molecular condensations as well as clusters of young stellar objects ( YSOs ) are identified in the N37 cloud , revealing ongoing star formation ( SF ) activities .
However , the analysis of ages of YSOs and the dynamical age of the H ii region do not support the origin of SF due to the influence of OB stars .
The position-velocity analysis of ^ { 13 } CO data reveals that two molecular clouds are inter-connected by a bridge-like structure , favoring the onset of a cloud-cloud collision process .
The SF activities ( i.e .
the formation of YSOs clusters and OB stars ) in the N37 cloud are possibly influenced by the cloud-cloud collision .