A Theory for the Excitation of CO in Star Forming Galaxies
  Observations of molecular gas in high-z star-forming galaxies typically rely
on emission from CO lines arising from states with rotational quantum numbers J
> 1. Converting these observations to an estimate of the CO J=1-0 intensity,
and thus inferring H2 gas masses, requires knowledge of the CO excitation
ladder, or spectral line energy distribution (SLED). The few available multi-J
CO observations of galaxies show a very broad range of SLEDs, even at fixed
galaxy mass and star formation rate, making the conversion to J=1-0 emission
and hence molecular gas mass highly uncertain. Here, we combine numerical
simulations of disk galaxies and galaxy mergers with molecular line radiative
transfer calculations to develop a model for the physical parameters that drive
variations in CO SLEDs in galaxies. An essential feature of our model is a
fully self-consistent computation of the molecular gas temperature and
excitation structure. We find that, while the shape of the SLED is ultimately
determined by difficult-to-observe quantities such as the gas density,
temperature, and optical depth distributions, all of these quantities are
well-correlated with the galaxy's mean star formation rate surface density
(Sigma_SFR), which is observable. We use this result to develop a model for the
CO SLED in terms of Sigma_SFR, and show that this model quantitatively
reproduces the SLEDs of galaxies over a dynamic range of ~200 in SFR surface
density, at redshifts from z=0-6. This model should make it possible to
significantly reduce the uncertainty in deducing molecular gas masses from
observations of high-J CO emission.
