This is something of a repeat of yesterday's exercise, but for Herschel data on larger scales, where filamentation is expected (at different angles?) on a different scale than the Galactic plane. First example: L030 500 microns

There is evidently a preferred direction that is correlated down to the resolution of the map, though the preference is smallest at the smallest scales. This may simply be a statement that there are more sources along the galactic plane, though, since there really isn't any particularly obvious filamentation in the image.

In L59, on the other hand, there is at most a very weak preference except at the largest scales corresponding to the Galactic Plane. This is somewhat interesting because there IS obvious filamentation in the L59 image, but it does not have a preferred direction. Unfortunately, it is not obvious whether or where filamentation shows up in fourier space if it does not have a preferred direction. There is no excess at any spatial scale that I can pick out.