Speaker
Daniel Haydon
(Astronomisches Rechen-Institut, University of Heidelberg (ARI/ZAH), Germany)
Description
A major problem in star/cluster formation and feedback is to constrain the
cloud-scale physics across galactic environment and cosmic time. A promising solution
has been put forward by Kruijssen & Longmore (2014), who present a statistical method
for measuring ill-constrained cloud-scale quantities such as the cloud lifetime, star
formation / feedback time-scales, star formation efficiencies, feedback velocities,
and mass loading factors, using galaxy-scale observations. I will use detailed
hydrodynamical simulations of disc galaxies to demonstrate that the method accurately
retrieves the above quantities down to an uncertainty of just a few 10%, but only if
the characteristic "reference timescale" of the star formation tracer is known. I
will then use synthetic H alpha, NUV, and FUV maps of the simulated galaxies to
measure their reference timescales and demonstrate that we constrain them to high
accuracy. I will also show that these time scales are environmentally dependent as
predicted by IMF theory. These results enable the first observational census of
cloud-scale star formation / feedback physics in galaxies across cosmic time.
Primary author
Daniel Haydon
(Astronomisches Rechen-Institut, University of Heidelberg (ARI/ZAH), Germany)
