  We review the coronal visible and infrared lines, collecting previous
observations, and comparing, whenever available, observed radiances with those
predicted by various models: the quiet Sun, a moderately active Sun, and an
active region as observed near the limb, around 1.1R$_{\odot}$. We also model
the off-limb radiances for the quiet Sun case. We used the most up-to-date
atomic data in CHIANTI version 8. The comparison is satisfactory, in that all
of the strong visible lines now have a firm identification. We revise several
previous identifications and suggest some new ones. We also list the large
number of observed lines for which we do not currently have atomic data, and
therefore still await firm identifications. We also show that a significant
number of coronal lines should be observable in the near-infrared region of the
spectrum by the upcoming Daniel K. Inouye Solar Telescope (DKIST) and the
AIR-Spec instrument, which observed the corona during the 2017 August 21 solar
eclipse. We also briefly discuss the many potential spectroscopic diagnostics
available to the visible and infrared, with particular emphasis on measurements
of electron densities and chemical abundances. We briefly point out some of the
potential diagnostics that could be available with the future infrared
instrumentation that is being built for DKIST and planned for the
  Coronal Solar Magnetism Observatory (COSMO). Finally, we highlight the need
for further improvements in the atomic data.
