24 | | Federath sent me a CDM of his turb+grav+mag+jets run. This was a fits file, whose pixel values represented column density in units of g/cm^2^. Ds9 showed the values ranged between 0 and ~2.5. Amira doesn't take fits files, but can process image formats. So I opened the fits in gimp and then exported it as a tiff file, and read this version into Amira. This apparently rescaled the data, as you can see from this histogram of voxel values: |
25 | | |
26 | | [[Image(FedHisto.png, 50%)]] |
27 | | [[Image(ds9histo.png, 50%)]] |
28 | | |
29 | | Now all the pixel values lay between 0 and about 66. This might have to do with the formatting of the tiff file (256 possible values in this format), but isn't overly important for skelatonization. If we wanted to do more in depth stats, might want to look into reading the data into Amira another way to preserve the absolute values of the voxels. |
30 | | |
45 | | There are a lot of clear filamentous structure that Amira is missing -- so I tried playing in the filament editor of Amira, which instead of a threshold now let's you auto trace using a windowing function. This windowing function lets you control contrast. |
46 | | |
47 | | [[Image(window1.png, 95%)]] |
48 | | |
49 | | [[Image(windo2.png, 95%)]] |
50 | | |
51 | | [[Image(windo3.png, 95%)]] |
52 | | |
53 | | [[Image(windo4.png, 95%)]] |
54 | | |
55 | | [[Image(windo5.png, 95%)]] |
56 | | |
57 | | This suggests that the first way of doing the tracing was using also using contrast, through the color map perhaps. Then you adjusted a threshold for this. If this is the case, using contrast lets you control what filament to capture. Playing with the 'window' let me trace some filaments in the bubbles. Looking at the Fig. 5 in the algorithm paper (Fouard et al 2006) also seems to suggest contrast is what is being traced. |
| 37 | There are a lot of clear filamentous structure that Amira is missing. |