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Aims. We aim to study the structure and kinematics of the two filamentsinside the subsonic core Barnard 5 in Perseus using high-resolution ($\approx$2400 au) NH3 data and a multi-component fit analysis.  Methods. We used observations of NH3 (1,1) and (2,2) inversion transitionsusing the Very Large Array (VLA) and the Green Bank Telescope (GBT). Wesmoothed the data to a beam of 8'' to reliably fit multiple velocity componentstowards the two filamentary structures identified in B5.  Results. Along with the core and cloud components, which dominate the flux inthe line of sight, we detected two components towards the two filaments showingsigns of infall. We also detected two additional components that can possiblytrace new material falling into the subsonic core of B5.  Conclusions. Following comparison with previous simulations of filamentformation scenarios in planar geometry, we conclude that either the formationof the B5 filaments is likely to be rather cylindrically symmetrical or thefilaments are magnetically supported. We also estimate infall rates of$1.6\times10^{-4}\,M_\odot\,yr^{-1}$ and $1.8\times10^{-4}\,M_\odot\,yr^{-1}$(upper limits) for the material being accreted onto the two filaments. At theserates, the filament masses can change significantly during the core lifetime.We also estimate an upper limit of $3.5\times10^{-5}\,M_\odot\,yr^{-1}$ for therate of possible infall onto the core itself. Accretion of new material ontocores indicates the need for a significant update to current core evolutionmodels, where cores are assumed to evolve in isolation.

Infall of material onto the filaments in Barnard 5