HOT-SPOTS IN THE NGC-2071 MOLECULAR OUTFLOW

In this Letter we present high spatial resolution (7'') images, obtained with the Berkeley-Illinois-Maryland Association (BIMA) interferometer, of the 47-66 km s(-1) CO J = 1-0 emission in the redshifted lobe of the NGC 2071 molecular outflow. The 47-66 km s(-1) CO, hereafter referred to as the extremely high velocity (EHV) feature, has mass 0.01 M., temperature 50 K, and density 2 x 10(5) cm(-3), and is spatially compact and spectrally distinct from the swept-up flow (3.5 M.). The EHV emission region consists of three main peaks which are individually unresolved by the interferometer beam. The EHV peaks resemble the ''hot spots'' found in the lobes of extragalactic radio sources. Since the EHV emission does not trace the outline of any of the known clumps in the outflow lobe, the EHV emission cannot be modeled as clumps being accelerated by a wind. Instead, we propose that the hot spots are caused by the (unseen) jet striking a known clump; either the jet bow shock fragments, or there are multiple bow shocks formed by a wandering jet.