Local HI filaments driven by a small-scale dynamo. Update on the velocity decomposition algorithm

TL;DR

This study investigates the coherence between far-infrared and HI filaments, revealing that their alignment and curvature are consistent with magnetic field structures influenced by a small-scale turbulent dynamo.

Contribution

We demonstrate that HI and FIR filaments are coherent structures with specific velocity and curvature properties, supporting models of magnetic field organization by a small-scale dynamo.

Findings

High polarization fractions up to 80% observed in HI filaments.

Filament orientations are correlated with velocity within narrow intervals.

Filament bending aligns with magnetic field curvature models.

Abstract

Context. HI 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 HI 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 HI on angular scales of 18 arcmin. Methods. We use HI4PI HI 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 HI. Results. We find some correlation for HI column densities at |v_LSR | < 50 km/, but a tight agreement between FIR and HI orientation angles {\theta} exists only in narrow velocity intervals of 1 km/s. Accordingly, we assign velocities to FIR filaments. Along the line of sight these HI 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 HI 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 HI and FIR filaments identified by the Hessian analysis are coherent structures with well-defined radial velocities. HI 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.