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We present findings of 3D filamentary structures in the Smith Cloud, ahigh-velocity cloud (HVC) located at $l=38^{\circ}$, $b=-13^{\circ}$. We usedata from the Galactic Arecibo L-Band Feed Array \ion{H}{i} (GALFA-\ion{H}{i})along with our new filament detection algorithm, \texttt{fil3d}, tocharacterize these structures. In this paper, we also discuss how differentinput parameters affect the output of \texttt{fil3d}. We study filaments in thelocal ISM and compare them to those found in the Smith Cloud. Based on thermallinewidth estimations we find supporting evidence that the Smith Cloudfilaments are part of its warm neutral medium. We also find a relationshipbetween thermal linewidth and the $v_{LSR}$ of the filaments. We study theplane-of-sky magnetic field as traced by Planck 353 GHz polarized dust emissionalong the line of sight and find the HI filaments in this region are notaligned with the magnetic field. This is likely related to their location closeto dynamic processes in the Galactic Plane and/or the low column density of thefilaments relative to emission in the Plane. The results show the HI filamentsare found in a wide range of Galactic environments and form through multipleprocesses.

Properties of 3D HI Filaments in the Smith High Velocity Cloud