Many crucial emission lines probing cloud evolution (e.g., CI) and
star formation (high-frequency N2H+ and CO, H2D+) can only be observed
at high frequencies. Such line emission is usually extended. Our
Cygnus-X maps, e.g., reveal that N2H+ and H2D+ covers areas >>1pc in
length (Pillai et al., ApJ, submitted). Yet the most relevant star
formation processes occur on the scale of individual cores
(<0.1pc). CCAT's well-resolved wide-field line maps will reveal
structure on all these scales. It is not possible to fully exploit
these data by treating clouds as sets of "cores" and "clumps". We must
adopt data analysis approaches that embrace the full complexity of
cloud structure. We have demonstrated this with tree-based
hierarchical cloud segmentation schemes (Kauffmann et al. 2010a,b,c,
ApJ), and we now study wide-field line maps similar to those that will
be produced by CCAT (Kauffmann et al., in prep.). I discuss how CCAT
data analysis can benefit from such approaches.