  The depletion of elements onto dust grains is characterized using a
generalized depletion strength $F_*$ for any sightline, and trend-line
parameters $A_X, B_X$ and $z_X$. The parameters $A_X, B_X$ and $z_X$ define the
relative depletion pattern, for which values are published in previous works.
The present study uses these parameters to calculate post-depleted gas-phase
abundances of 15 different elements while varying $F_*$ from 0 to 1. An
analysis of emergent strong spectral line intensities, obtained by inputting
the calculated abundances into a cloudy model, shows that the depletion
strength has a non-trivial effect on predicted emission lines and the thermal
balance of the ionized cloud. The amount by which elements deplete also affects
the coolant abundances in the gas. Furthermore, it was found that each of the
parameters - metallicity, ionization parameter U and depletion strength $F_*$
have degenerate effects on the emission-line strengths, and thermal balance of
the interstellar medium (ISM). Finally, comparing our results to a sample of H
II regions using data obtained from the Mapping Nearby Galaxies at Apache Point
Observatory survey (MaNGA) revealed that the best-fit $F_*$ was approximately
0.5. However, this best-fit value does not work well for all metallicities.
Removing the sulfur depletion and changing the nitrogen abundance pattern can
improve the fit. As a result, extra observational evidence is required to
verify the choices of parameters and better constrain the typical depletion
strength in galaxies.
