  The Early Universe Molecular Emission Line Galaxies (EMGs) are a population
of galaxies with only 36 examples that hold great promise for the study of
galaxy formation and evolution at high redshift. The classification, luminosity
of molecular line emission, molecular mass, far-infrared (FIR) luminosity, star
formation efficiency, morphology, and dynamical mass of the currently known
sample are presented and discussed. The star formation rates derived from the
FIR luminosity range from about 300 to 5000 M(sun)per year and the molecular
mass from 4 x 10^9 to 1 x 10^{11} M(sun). At the lower end, these star
formation rates, gas masses, and diameters are similar to those of local
ultraluminous infrared galaxies, and represent starbursts in centrally
concentrated disks, sometimes, but not always, associated with active galactic
nuclei. The evidence for large (> 5 kpc) molecular disks is limited. Morphology
and several high angular resolution images suggest that some EMGs are mergers
with a massive molecular interstellar medium in both components. A critical
question is whether the EMGs, in particular those at the higher end of the gas
mass and luminosity distribution, represent the formation of massive, giant
elliptical galaxies in the early Universe. The sample size is expected to grow
explosively in the era of the Atacama Large Millimeter Array (ALMA).
