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We present a comprehensive analysis of the Galactic mid-infrared (MIR) bubble[HKS2019] E70 (E70) by adopting a multi-wavelength approach to understand thephysical environment and star formation scenario around it. We identified asmall (radius ~1.7 pc) stellar clustering inside the E70 bubble and itsdistance is estimated as 3.26 +/- 0.45 kpc. This cluster is embedded in themolecular cloud and hosts massive stars as well as young stellar objects(YSOs), suggesting active star formation in the region. The spectral type ofthe brightest star 'M1' of the E70 cluster is estimated as O9V and a circularring/shell of gas and dust is found around it. The diffuse radio emissioninside this ring/shell, the excess pressure exerted by the massive star 'M1' atthe YSOs core, and the distribution of photo-dissociation regions (PDRs), aClass I YSO, and two ultra-compact (UC) H II regions on the rim of thisring/shell, clearly suggest positive feedback of the massive star 'M1' in theregion. 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 velocitystructure of the 12 CO emission suggests that the feedback from the massivestar appears to have expelled the molecular material and subsequent swept-upmaterial is what appears as the E70 bubble.

Exploring Stellar Cluster and Feedback-driven Star Formation in Galactic Mid-infrared Bubble [HKS2019] E70