direction, with the outer lobes symmetrically separated from the central source by an angular distance of $\sim10{''}$, equivalent to a physical separation in the plane of the sky of $\sim$0.14 pc. The positive spectral index of the central source is consistent with that expected for a radio thermal (free-free) jet (e.g., Anglada 1996; Rodríguez 1997), while the spectral index of the lobes suggests a mix of thermal and nonthermal emission. Forster & Caswell (1989) detected both mainline OH and H$_2$O masers at a position close to the central continuum source. The triple system is centered on the position of the IRAS source and is also coincident within measurement error with a 1.2 mm dust continuum and molecular line emission core whose mass is on the order of 10$^3$ $M_\odot$ (Garay et al. 2003). Brooks et al. (2003) reported a chain of $H_2$ 2.12 $\mu$m emission knots that trace a collimated flow extending over 1.5 pc that emanates from close to the central component of the triple radio source and has a position angle very similar to that defined by the outer lobes of the triple radio source. Most likely this extended component traces gas ejected in the past by the 