  We identify a molecular bubble, and study the star formation and its feedback
in the S Mon region, using multiple molecular lines, young stellar objects
(YSOs), and infrared data. We revisit the distance to S Mon, ~722+/-9 pc, using
Gaia Data Release 3 parallaxes of the associated Class II YSOs. The bubble may
be mainly driven by a massive binary system (namely 15 Mon), the primary of
which is an O7V-type star. An outflow is detected in the shell of the bubble,
suggesting ongoing star formation activities in the vicinity of the bubble. The
total wind energy of the massive binary star is three orders of magnitude
higher than the sum of the observed turbulent energy in the molecular gas and
the kinetic energy of the bubble, indicating that stellar winds help to
maintain the turbulence in the S Mon region and drive the bubble. We conclude
that the stellar winds of massive stars have an impact on their surrounding
environment.
