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kruijssen edited section_SMA_CMZ_8_GHz__.tex
about 9 years ago
Commit id: 23a03d6aab306fb23b97cd4c29ce9e828c8cd604
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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, 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.