Distance to Sh2-106 from Gaia DR3 and its embedded radio population: implications for a candidate explosive outflow

Sh2-106 has recently been proposed as a candidate explosive molecular outflow (EMO), but the physical interpretation of the region depends critically on its distance. Published estimates span a wide range, leading to large uncertainties in the inferred size, energetics, and evolutionary timescale of the system. Using Gaia DR3 astrometry, we identify a kinematically coherent stellar population associated with Sh2-106 and derive a cluster parallax of corr=0.607 plus or minus0.013,mas, corresponding to a distance of 1.65 plus or minus0.04,kpc. This value is significantly larger than the commonly adopted extinction-break estimate of 1.09,kpc. At this revised distance, the inferred kinetic energy of the expanding ionized nebula increases by a factor of about6.5, reaching E exp 1.3 times10 48,erg and placing Sh2-106 in the same order-of-magnitude energetic regime as the Orion BN/KL explosive event, although at a substantially older dynamical age (about3500,yr). Archived 5.8,GHz Karl G. Jansky Very Large Array observations reveal ten compact radio sources in the central region, identifying embedded stellar objects that are suitable for future multi-epoch radio astrometry. No unambiguous high-velocity stellar ejecta are detected in Gaia DR3, although S106,IR shows a modest peculiar transverse velocity of about5,km,s-1 relative to the cluster centroid. The Gaia-based cluster distance, therefore, significantly revises the physical scale and energetics of Sh2-106 and provides the observational framework required to test whether the region represents an older analogue of the Orion BN/KL dynamical disintegration or a distinct explosive phenomenon.