  High-spatial-resolution HI observations have led to the realisation that the
nearby (within few hundreds of parsecs) Galactic atomic filamentary structures
are aligned with the ambient magnetic field. Enabled by the high quality data
from the Australian Square Kilometre Array Pathfinder (ASKAP) radio telescope
for the Galactic ASKAP HI (GASKAP-HI) survey, we investigate the potential
magnetic alignment of the $\gtrsim 10\,{\rm pc}$-scale HI filaments in the
Small Magellanic Cloud (SMC). Using the Rolling Hough Transform (RHT) technique
that automatically identifies filamentary structures, combined with our newly
devised ray-tracing algorithm that compares the HI and starlight polarisation
data, we find that the HI filaments in the northeastern end of the SMC main
body ("Bar" region) and the transition area between the main body and the tidal
feature ("Wing" region) appear preferentially aligned with the magnetic field
traced by starlight polarisation. Meanwhile, the remaining SMC volume lacks
starlight polarisation data of sufficient quality to draw any conclusions. This
suggests for the first time that filamentary HI structures can be magnetically
aligned across a large spatial volume ($\gtrsim\,{\rm kpc}$) outside of the
Milky Way. In addition, we generate maps of the preferred orientation of HI
filaments throughout the entire SMC, revealing the highly complex gaseous
structures of the galaxy likely shaped by a combination of the intrinsic
internal gas dynamics, tidal interactions, and star formation feedback
processes. These maps can further be compared with future measurements of the
magnetic structures in other regions of the SMC.
