  Gaia DR3 and further releases have the potential to identify and categorise
new emission-line stars in the Galaxy. We perform a comprehensive validation of
astrophysical parameters from Gaia DR3 with the spectroscopically estimated
emission-line star parameters from LAMOST OBA emission catalogue. We compare
different astrophysical parameters provided by Gaia DR3 with those estimated
using LAMOST spectra. By using a larger sample of emission-line stars, we
perform a global polynomial and piece-wise linear fit to update the empirical
relation to convert Gaia DR3 pseudo-equivalent width to observed equivalent
width, after removing the weak emitters from the analysis. We find that the
emission-line source classifications given by DR3 is in reasonable agreement
with the classification from LAMOST OBA emission catalogue. The astrophysical
parameters estimated by esphs module from Gaia DR3 provides a better estimate
when compared to gspphot and gspspec. A second-degree polynomial relation is
provided along with piece-wise linear fit parameters for the equivalent width
conversion. We notice that the LAMOST stars with weak H{\alpha} emission are
not identified to be in emission from BP/RP spectra. This suggests that
emission-line sources identified by Gaia DR3 is incomplete. In addition, Gaia
DR3 provides valuable information about the binary and variable nature of a
sample of emission-line stars.
