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Detection of a turbulent gas component associated with a starless core with subthermal turbulence in the Orion A cloud

We report the detection of a wing component in NH$_3$ emission toward the starless core TUKH122 with subthermal turbulence in the Orion A cloud. This NH$_3$ core is suggested to be on the verge of star formation because the turbulence inside the NH$_3$ core is almost completely dissipated, and also because it is surrounded by CCS, which resembles the prestellar core L1544 in Taurus showing infall motions. Observations were carried out with the Nobeyama 45 m telescope at 0.05 km s$^{-1}$ velocity resolution. We find that the NH$_3$ line profile consists of two components. The quiescent main component has a small linewidth of 0.3 km s$^{-1}$ dominated by thermal motions, and the red-shifted wing component has a large linewidth of 1.36 km s$^{-1}$ representing turbulent motions. These components show kinetic temperatures of 11 K and $<$ 30 K, respectively. Furthermore, there is a clear velocity offset between the NH$_3$ quiescent gas ($VLSR=3.7$ km s$^{-1}$) and the turbulent gas ($VLSR=4.4$ km s$^{-1}$). The centroid velocity of the turbulent gas corresponds to that of the surrounding gas traced by the $^{13}$CO ($J=1-0$) and CS ($J=2-1$) lines. LVG model calculations for CS and CO show that the turbulent gas has a temperature of $8-13$ K and an H$_2$ density of ~ $10^4$ cm$^{-3}$, suggesting that the temperature of the turbulent component is also ~ 10 K. The detections of both NH$_3$ quiescent and wing components may indicate a sharp transition from the turbulent parent cloud to the quiescent dense core.