Using the short-high module of the Infrared Spectrograph on the Spitzer Space Telescope , we have measured the [ S iv ] 10.51 , [ Ne ii ] 12.81 , [ Ne iii ] 15.56 , and [ S iii ] 18.71- \mu m emission lines in nine H ii regions in the dwarf irregular galaxy NGC 6822 . These lines arise from the dominant ionization states of the elements neon ( Ne ^ { + + } , Ne ^ { + } ) and sulphur ( S ^ { 3 + } , S ^ { + + } ) , thereby allowing an analysis of the neon to sulphur abundance ratio as well as the ionic abundance ratios Ne ^ { + } /Ne ^ { + + } and S ^ { 3 + } /S ^ { + + } . By extending our studies of H ii regions in M83 and M33 to the lower metallicity NGC 6822 , we increase the reliability of the estimated Ne/S ratio . We find that the Ne/S ratio appears to be fairly universal , with not much variation about the ratio found for NGC 6822 : the median ( average ) Ne/S ratio equals 11.6 ( 12.2 \pm 0.8 ) . This value is in contrast to Asplund et al. ’ s currently best estimated value for the Sun : Ne/S = 6.5 . In addition , we continue to test the predicted ionizing spectral energy distributions ( SEDs ) from various stellar atmosphere models by comparing model nebulae computed with these SEDs as inputs to our observational data , changing just the stellar atmosphere model abundances . Here we employ a new grid of SEDs computed with different metallicities : Solar , 0.4 Solar , and 0.1 Solar . As expected , these changes to the SED show similar trends to those seen upon changing just the nebular gas metallicities in our plasma simulations : lower metallicity results in higher ionization . This trend agrees with the observations .