Biases and Cosmic Variance in Molecular Gas Abundance Measurements
  Recent deep millimeter-wave surveys attempt to measure the carbon monoxide
(CO) luminosity function and mean molecular gas density through blind
detections of CO emission lines. While the cosmic star formation rate density
is now constrained in fields hundreds of arcmin$^2$ or more, molecular gas
studies have been limited to $\le50$ arcmin$^2$. These small fields result in
significant biases that have not been accounted for in published results. To
quantify these biases, we assign CO luminosities to halos in cosmological
simulations to produce mock observations for a range of field sizes. We find
that fields $\lesssim 10$ arcmin$^2$ alter the recovered shape of the
luminosity function, causing underestimates of the number of bright objects.
Our models suggest that current surveys are sensitive enough to detect sources
responsible for approximately half of the cosmic molecular gas density at high
redshift. However, uncertainties in the gas density measurement are large, and
cosmic variance may double the uncertainty claimed in these surveys. As a
result, the field size needed to detect redshift evolution in the molecular gas
at high confidence may be more than an order of magnitude larger than what
current surveys have achieved. Shot power intensity mapping measurements are
particularly sensitive to Poisson variance and require yet larger areas to
constrain the gas density or its evolution. We provide a simple prescription
for approximating uncertainty in total CO emission as a function of survey area
and redshift, for both direct detection and intensity mapping surveys.
