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High-resolution observations of the Perseus B5 "core" have previouslyrevealed that this subsonic region actually consists of several filaments thatare likely in the process of forming a quadruple stellar system. Since subsonicfilaments are thought to be produced at the $\sim 0.1$ pc sonic scale byturbulent compression, a detailed kinematic study is crucial to test such ascenario in the context of core and star formation. Here we present a detailedkinematic follow-up study of the B5 filaments at a 0.009 pc resolution usingthe VLA and GBT combined observations fitted with multi-component spectralmodels. Using precisely identified filament spines, we find a remarkableresemblance between the averaged width profiles of each filament andPlummer-like functions, with filaments possessing FWHM widths of $\sim 0.03$pc. The velocity dispersion profiles of the filaments also show decreasingtrends towards the filament spines. Moreover, the velocity gradient field in B5appears to be locally well ordered ($\sim 0.04$ pc) but globally complex, withkinematic behaviors suggestive of inhomogeneous turbulent accretion ontofilaments and longitudinal flows towards a local overdensity along one of thefilaments.

Turbulence and Accretion: a High-resolution Study of the B5 Filaments