Local H I filaments driven by a small-scale dynamo Unraveling the velocities and tangling of dusty magnetized structures

Context. H I filaments are closely related to dusty magnetized structures that are observable in the far infrared (FIR). Recently it was proposed that the coherence of oriented H I structures in velocity traces the line of sight magnetic field tangling. Aims. We study the velocity-dependent coherence between FIR emission at 857 GHz and H I on angular scales of 18 '. Methods. We use HI4PI H I data and Planck FIR data and apply the Hessian operator to extract filaments. For coherence, we require that local orientation angles theta in the FIR at 857 GHz along the filaments be correlated with the H I. Results. We find some correlation for H I column densities at |v(LSR)| < 50 km s(-1), but a tight agreement between FIR and H I orientation angles theta exists only in narrow velocity intervals of 1 km s(-1). Accordingly, we assign velocities to FIR filaments. Along the line of sight these H I structures show a high degree of the local alignment with theta, as well as in velocity space. Interpreting these aligned structures in analogy to the polarization of dust emission defines an H I polarization. We observe polarization fractions of up to 80%, with averages of 30%. Orientation angles theta along the filaments, projected perpendicular to the line of sight, are fluctuating systematically and allow a characteristic distribution of filament curvatures to be determined. Conclusions. Local H I and FIR filaments identified by the Hessian analysis are coherent structures with well-defined radial velocities. H I structures are also organized along the line of sight with a high degree of coherence. The observed bending of these structures in the plane of the sky is consistent with models for magnetic field curvatures induced by a Galactic small-scale turbulent dynamo.