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We present Herschel, ALMA Compact Array (ACA), and Caltech SubmillimeterObservatory (CSO) observations of the prestellar core in L1689N, which has beensuggested to be interacting with a molecular outflow driven by the nearby solartype protostar IRAS 16293-2422. This source is characterized by some of thehighest deuteration levels seen in the interstellar medium. The change in theNH2D line velocity and width across the core provides clear evidence of aninteraction with the outflow, traced by the high-velocity water emission.Quiescent, cold gas, characterized by narrow line widths is seen in the NE partof the core, while broader, more disturbed line profiles are seen in the W/SWpart. Strong N2D+ and ND3 emission is detected with the ACA, extending S/SWfrom the peak of the single-dish NH2D emission. The ACA data also reveal thepresence a compact dust continuum source, with a mean size of ~1100 au, acentral density of (1-2) 10^7 cm-3, and a mass of 0.2-0.4 Msun. The dustemission peak is displaced ~5" to the south with respect to the N2D+ and ND3emission, as well as the single-dish dust continuum peak, suggesting that thenorthern, quiescent part of the core is characterized by spatially extendedcontinuum emission, which is resolved out by the interferometer. We see noclear evidence of fragmentation in this quiescent part of the core, which couldlead to a second generation of star formation, although a weak dust continuumsource is detected in this region in the ACA data.

Star Formation and Feedback: A Molecular Outflow-Prestellar Core Interaction in L1689N