The Molecular Core and the Powering Source of the Bipolar Molecular Outflow in NGC 2264G

We present NH3 (1, 1) and (2, 2), and radio continuum observations toward the bipolar molecular outflow NGC 2264G. We detected a high-density NH3, core of 0.08 x 0.06 pc in size, M approximately = 6(X_NH3/10^-8-1 solar mass, and T_K approximately = 15 K, located almost midway between the blueshifted and redshifted CO lobes of the outflow. Neither the infrared sources detected so far (with the exception of IRAS 06384+0958) nor very large array (VLA) 1, the radio continuum source previously detected in the area (and suggested as the powering source of the outflow), appears to be associated with the high-density molecular clump. However, we detected a new radio continuum source, VLA 2, close to the maximum of NH3 emission. This continuum source shows a jetlike morphology, elongated in the direction of the bipolar molecular outflow. We propose that VLA 2 is a deeply embedded low-mass star and the most likely powering source of the bipolar outflow in NGC 2264G. We find that the mechanical luminosity of the wind from from VLA 2 is of the same order as the mechanical luminosity of the outflow, and as the estimated stellar luminosity of the source. Thus, this remarkable source appears to provide a very efficient outflow acceleration mechanism.