Rydberg States of H$_3$ and HeH as Potential Coolants for Primordial
  Star Formation
  Current theory and measurements establish the age of the universe as ca. 13.8
billion years. For the first several hundred million years of its existence, it
was a dark, opaque void. After that, the hydrogen atoms comprising most of the
"ordinary" matter began to condense and ionize, eventually forming the first
stars that would illuminate the sky. Details of how these "primordial" stars
formed have been widely debated, but remain elusive. A central issue in this
process is the mechanism by which the primordial gas (mainly hydrogen and
helium atoms) collected via the action of dark matter cools and further
accretes to fusion densities. Current models invoke collisional excitation of
H$_2$ molecular rotations and subsequent radiative rotational transitions
allowed by the weak molecular quadrupole moment. In this article, we review the
salient considerations, and present some new ideas, bases on recent
spectroscopic observations of neutral H$_3$ Rydberg electronic state emission
in the mid-infrared.
