  Stellar, substellar, and planetary atmosphere models are all highly sensitive
to the input opacities. Generational differences between various
state-of-the-art stellar/planetary models are primarily because of incomplete
and outdated atomic/molecular line-lists. Here we present a database of
pre-computed absorption cross-sections for all isotopologues of key atmospheric
molecules relevant to late-type stellar, brown dwarf, and planetary
atmospheres: MgH, AlH, CaH, TiH, CrH, FeH, SiO, TiO, VO, and H2O. The pressure
and temperature ranges of the computed opacities are between
10$^{-6}$--3000~bar and 75--4000~K, and their spectral ranges are
0.25--330~$\mu$m for many cases where possible. For cases with no
pressure-broadening data, we use collision theory to bridge the gap. We also
probe the effect of absorption cross-sections calculated from different line
lists in the context of Ultra-Hot Jupiter and M-dwarf atmospheres. Using 1-D
self-consistent radiative-convective thermochemical equilibrium models, we
report significant variations in the theoretical spectra and thermal profiles
of substellar atmospheres. With a 2000 K representative Ultra-Hot Jupiter, we
report variations of up to 320 and 80 ppm in transmission and thermal emission
spectra, respectively. For a 3000 K M-dwarf, we find differences of up to
125$\%$ in the spectra. We find that the most significant differences arise due
to the choice of TiO line-lists, primarily below 1$\mu$m. In sum, we present
(1) a database of pre-computed molecular absorption cross-sections, and (2)
quantify biases that arise when characterizing substellar/exoplanet atmospheres
due to line list differences, therefore highlighting the importance of correct
and complete opacities for eventual applications to high precision spectroscopy
and photometry.
