  The infrared solar spectrum contains a wealth of physical data about the Sun
and is being explored using modern detectors and technology with new
ground-based solar telescopes. One such instrument will be the ground-based
Cryogenic Near-IR Spectro-Polarimeter of the Daniel K. Inouye Solar Telescope
that will be capable of sensitive imaging of the faint infrared solar coronal
spectra with full Stokes I, Q, U, and V polarization states. Highly ionized
magnetic dipole emission lines have been observed in galaxies and the solar
corona. Quantifying the accuracy of spectral inversion procedures requires a
precise spectroscopic calibration of observations. A careful interpretation of
the spectra around prominent magnetic dipole lines is essential for deriving
physical parameters, and particularly, for quantifying the off-limb solar
coronal observations from DKIST. In this work, we aim to provide an analysis of
the spectral regions around the infrared coronal emission lines of Fe XIII
1074.68 nm, Fe XIII 1079.79 nm, Si X 1430.10 nm, and Si IX 3934.34 nm, aligning
with the goal of identifying solar photospheric and telluric lines that will
help facilitate production of reliable inversions and data products from four
sets of solar coronal observations. The outputs will be integrated in the
processing pipeline to produce Level-2 science-ready data that will be made
available to DKIST observers.
