velocity dispersion vs density?
+ high redshift clouds and CMZ clouds occupy same parameter space
"CMZ is inditinguishable from high-redshift starburst"
Details of stellar mass assembly
Molinari Ring picture: 2 vertical oscillations per orbit
map mass density along orbit
gas compressed at pericenter
PPV structure extraction...
+ orbital fitting
+ can't fit Molinari ring
+ closed orbits not possible: precession
+ can't fit P-V wiggle
+ doesn't fit Sgr B2
Pericenter passage SPH sim
+ VERTICAL compression
+ retrograde, counterrotating gas due to shear
dense gas fraction vs orbit...
+ prediction of density vs orbital position
+ Plug for Ginsburg et al VLA/GBT H2CO densitometry
IMF variation interesting future avenue
Questions
Q: On pc scales, fits with Ken-Schmidt relation
A: Depends on geometry. Donut vs pancake geometry.
Q: Isn't there gas that is more efficient at forming stars?
A: Doesn't fit...
Q: KS relation doesn't work for CMZs in other galaxies. How did you measure
dispersion for high-Z clouds?
A: Some high-z clouds with direct measurements. Otherwise, assume virial
equilibrium. Robust no matter how you derive it.
Q: Struggling in nearby galaxies, particularly because of outflows.
A: best we can do
Q: CMZ is similar to high-z objects. GC in pre-starburst phase. So we
should have a starburst soon.
A: Either gas won't form stars, or will do so in bursty fashion
Q: Predicts lots of very dense gas in Galactic center, n~10^8.
A: See Jill's talk.
Q Wardle: Turbulence damps on vertical crossing time (0.5 Myr). 20km/s
linewidth disappear in 0.5 Myr? Do you see dead clouds? Don't travel very far,
so should damp.