  In a recent study, Banerjee et al. (2021) produced an atlas of all major
emission lines found in a large sample of 115 Galactic field Be stars using the
2-m Himalayan Chandra Telescope (HCT) facility located at Ladakh, India. This
paper presents our further exploration of these stars to estimate the electron
density in their discs. Our study using Balmer decrement values indicate that
their discs are generally optically thick in nature with electron density (n_e)
in their circumstellar envelopes (CEs) being in excess of 10^13 cm^-3 for
around 65% of the stars. For another 19% stars, the average n_e in their discs
probably range between 10^12 cm^-3 and 10^13 cm^-3. We noticed that the nature
of the H{\alpha} and H\b{eta} line profiles might not influence the observed
Balmer decrement values (i.e. D_34 and D_54) of the sample of stars.
Interestingly, we also found that around 50% of the Be stars displaying D_34
greater than 2.7 are of earlier spectral types, i.e. within B0 -B3.
