Direct multiwavelength comparison of GCL morphology between LVM optical line emission from Hα and [S III] (top left, center), MeerKAT 1.284 GHz radio continuum (top right), mid-IR dust emission in the PAH dominated 8.0 μm (bottom left) and thermal dust 24 μm (bottom center), and ¹³CO molecular gas (bottom right). The morphology of the [S III] and radio lobe agrees quite well at high Galactic latitudes, and is encased in an outer shell of PAH emission, with warm dust still in the region interior. CO clouds are offset, outside the GCL boundary. The GCL is marked in a solid red line, and the compact and bright GCL-1 is also marked in a dashed red line.