deletions | additions       diff --git a/section_SMA_CMZ_8_GHz__.tex b/section_SMA_CMZ_8_GHz__.tex  index f45f2c7..f7bfdeb 100644  --- a/section_SMA_CMZ_8_GHz__.tex  +++ b/section_SMA_CMZ_8_GHz__.tex 
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How can we identify star forming cores? Original idea: hot core tracers + outflows. Does that work? CH$_3$OH masers, but incomplete/maybe just shock tracers?  Evolutionary sequence in massive cores seen in dust ridge clouds. Steve: free-fall times come from single-dish, large scale. Diederik: position along ridge dominates spread in density. (Comment by Diederik: I have now checked this quantitatively and it turns out both are actually similarly important -- from Table 2 in KDL15, \citet{Kruijssen2015a},  the time-scale spread is from 0.30 Myr post-pericentre to 0.74 post-pericentre (a factor of 2.5), whereas the density spread is factor of 4 => factor of 2 in free-fall time. So the position is somewhat more important, but not by much.) Lines mapped: H$_2$CO, C$^{18}$O, CH$_3$OH, $^{13}$CO, SiO.