kruijssen edited section_SMA_CMZ_8_GHz__.tex  about 9 years ago

Commit id: 3a5247977aa6119c2706cb1477a0fb9e643ac46b

deletions | additions      

       

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 that the position is indeed somewhat more important, but not by much. much  -- from Table 2 in \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.) Lines mapped: H$_2$CO, C$^{18}$O, CH$_3$OH, $^{13}$CO, SiO.