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\section{Scientific Justification}  Our recent analysis of far-infrared (Herschel) observations indicates a close relationship between the ubiquitous filamentary structures and star formation. Numerical simulations plus morphological evidence Herschel maps suggest that stars form through gravitational fragmentation in filaments. Analyses As explained below, recent analyses  of multi-scale, kinematically-resolved, observations of the B5 region in Perseus appear to show that gravitationally bound cores form from fragmenting filments relatively quickly (see below). quickly.  L1689B is analogous to B5 in that it offers a relatively simple case of a young pre-stellar core sitting on a single filament, with a velocity gradient along the filament at parsec scales. We propose VLA observations of NH_3 (1, 1) and (2, 2) line emission of L1689B in order to trace the kinematics from the filament to the core, and {\bf in order to examine the star forming and fragmentation processes in the filament at an early stage}. \subsection{The case of B5 in the Perseus molecular cloud}  B5 in the Perseus molecular cloud was identified as a young pre-stellar core. Herschel observations shows that B5 sits in a filamentary strcutre, which extends for \~ 2 pc. FCRAO observations of ^{12}CO (1-0) and ^{13}CO (1-0) line emission show that the B5 region has a complicated velocity structure with multiple velocity components along the line of sight. Later with GBT observations of NH_3 (1, 1) and (2, 2) hyperfine lines, B5 is found to have a sub-sonic velocity disperson, conforming to the theory of star formation in {\it coherent cores}. By combining the GBT and the VLA data of NH_3 hyperfine lines, Jaime et al. find fragmentation within the coherent core. This provides the first direct evidence of star formation through filament fragmentation. (See Fig. ?)