  We present a comprehensive analysis of the Galactic mid-infrared (MIR) bubble
[HKS2019] E70 (E70) by adopting a multi-wavelength approach to understand the
physical environment and star formation scenario around it. We identified a
small (radius ~1.7 pc) stellar clustering inside the E70 bubble and its
distance is estimated as 3.26 +/- 0.45 kpc. This cluster is embedded in the
molecular cloud and hosts massive stars as well as young stellar objects
(YSOs), suggesting active star formation in the region. The spectral type of
the brightest star 'M1' of the E70 cluster is estimated as O9V and a circular
ring/shell of gas and dust is found around it. The diffuse radio emission
inside this ring/shell, the excess pressure exerted by the massive star 'M1' at
the YSOs core, and the distribution of photo-dissociation regions (PDRs), a
Class I YSO, and two ultra-compact (UC) H II regions on the rim of this
ring/shell, clearly suggest positive feedback of the massive star 'M1' in the
region. We also found a low-density shell-like structure in 12 CO(J=1-0)
molecular emission along the perimeter of the E70 bubble. The velocity
structure of the 12 CO emission suggests that the feedback from the massive
star appears to have expelled the molecular material and subsequent swept-up
material is what appears as the E70 bubble.
