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We analyse the morphology and kinematics of dense filamentary structuresproduced in a numerical simulation of a star--forming cloud of $1.4 \times 10^4\, \Msun$ evolving under their own self--gravity in a magnetized medium. Thisstudy is motivated by recent observations of velocity--coherent substructures("fibres") in star-forming filaments. We find such "fibres" ubiquitously in oursimulated filament. We found that a fibre in one projection is not necessarilya fibre in another projection, and thus, caution should be taken into accountwhen considering them as real objects. We found that only the densest parts ofthe filament ($\sim$30\% of the densest volume, which contains $\sim$70\% ofthe mass) belong to fibres in 2 projections. Moreover, it is quite common thatthey are formed by separated density enhancements superposed along the line ofsight. Observations of fibres can yield insight into the level of turbulentsubstructure driven by gravity, but care should be taken in interpreting theresults given the problem of line of sight superposition. We also studied themorphology and kinematics of the 3D skeleton (spine), finding that subfilamentsaccrete structured material mainly along the magnetic field lines, which arepreferentially perpendicular to the skeleton. The magnetic field is at the sametime dragged by the velocity field due to the gravitational collapse.

Are fibres in molecular cloud filaments real objects?