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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, L1689B, in L1689 in the Ophiuchus molecular cloud, sits on a single filament that extends \~ 1.6 pc, and has an elongated shape along the filament direction (See Fig. ? for its morphology as observed by Herschel and on the 2MASS/NICER-based near-infrared extinction map). Like 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). L1689B 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}, cm^{-2} (Fig. ?),  both similar to B5 (\~ 10 K and \~ 2 to 5 $\times$ 10^{22} cm^{-2}). Despite the complicated velocity structures throughout L1689, L1689B and the filament it sits in seem to show some 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 to understand the star forming process in filaments. \subsection{Star formation in filaments}  Based on the Herschel results, Andr\'e et al. (2013) suggest that stars largely form in supercritical filaments, through three different modes of accretion (see Fig. ?): a) longitudinal infall along the main filament, b) radial infall across the main filament, and c) accretion of material from the background cloud through sub-filaments or {\it striations}, along the magnetic field lines. Kirk et al. (2013) further claim to find direct evidence of longitudinal infall along the main filament, through ATNF Mopra 22m observations of molecular line emission. While a few other observations also claim to see velocity gradient along/across the main filament, a more detailed analysis of the kinematics is needed to fully pin down the origins of these velocity gradient, and thus to test the paradigm of star formation in supercritical filaments provided by Andr\'e et al.