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Intriguingly, the projected morphology of the fragmented cores in B5 (with sizes of a few thousand AU) aligns well with the parsec-scale filament they sit in, as identified on the Herschel maps. This seems to suggest that the first stages of star forming process within filaments preserve the structure of the {\it mother filaments}. This is bizarre considering the difference in spatial scales between filaments (\~ a few parsec) and the condensations found by Jaime et al. (\~ a few thousand AU). To understand this phonomenon, it requires further analysis of the kinematics from the filament to the core and observations that are sensitive to the wide spatial scale range, of more young pre-stellar cores in filaments other than B5.  \subsection{L1689B: Another B5 or a differenct case?}  Similar to B5, the regions around L1689B (throughout the entire L1689) shows complicated velocity structures at parsec scales, as traced by ^{12}CO (1-0) and ^{13}CO (1-0) line emission (observed by FCRAO). It is classified as a young pre-stellar core, and has a temperature of \~ 10 K and a density of n_{H_2} \~ 2.6 $\times$ 10^{22} cm^{-2}, both similar to B5. On the Herschel far-infrared maps, it also appears to sit on a single filament that extends \~ 1.6 pc. However, despite pc, and has an elongated shape along the filament direction. Despite  the complicated velocity structures throughout L1689, L1689B and the filament it sits in seem to show some velcity velocity  gradient at the parsec scale, as observed by FCRAO. But again, limited by the resolution of the FCRAO data and further obscured by the complicated  velocity structures and the opacity, practical and quantitative analysis of kinematics using the FCRAO molecular line emission data is almost impossible. This emphasizes again the importance of molecular line observations that are sensitive to both the core and the filament scales, if we want o understand the star forming process in filaments. \subsection{Star formation in filaments}  \subsection{Proposed observation and immediate goal}  We propose to observe NH_3 (1, 1) and (2, 2) line emission (at 23.6945 GHz and 23.7226 GHz, respectively) around L1689B in the K band with the VLA D Array. To cover the full width of the filament (\~ 0.1 pc, corresponding to \~ 2.75 arcsec) and to trace velocity structures along the filament onto the core, we propose a mosaicking of 13 pointings. With a primary beam of size \~ 2 arcmin (full-width half-power), this allows us to cover 6 armin (\~ 0.22 pc) along the filament and 4 arcmin (\~ 0.15 pc) across the filament. (For reference  \subsection{Complementary data and planned analysis}