SIGAME can present the line emission from a galaxy in a space-velocity datacube format, which can be integrated in velocity to generate moment 0 maps such as the one in above for a z~0 merger in [CII].
By convolving a line emission map by the know beam size and shape of an instrument, a synthetic map can be generated and areas within a galaxy can be compared. In the figure above, this is done for a z~0 galaxy in [CII] emission, where the small yellow circles correspond to areas that Herschel would have been able to distinguish.
The radial profile in [CII] emission is calculated for different ISM phases (GMCs vs diffuse gas) by integrating the datacube in circular annuli around the center of the galaxy.
In order to compare with resolved observations of multiple lines, we are working on producing diagnostic contour maps, that can be used to convert line ratios into e.g. density and Far-UV flux (G0), as shown in the above figure.
In addition, SIGAME will take your galaxy (or galaxy sample) and collect numbers on galaxy global properties such as SFR, stellar mass, ISM mass, SFR-weighted metallicity etc. in one table stored as a dictionary. Then, line luminosities can be derived and added to that table for further use. However, the real power of SIGAME lies in the resolved spectral datacubes that can be converted into line profiles, line maps and much more, as shown above.