  In this study, we analyze the emission lines of different species present in
118 Galactic field classical Be stars in the wavelength range of 3800 - 9000
\AA. We re-estimated the extinction parameter (A$_V$) for our sample stars
using the newly available data from Gaia DR2 and suggest that it is important
to consider A$_V$ while measuring the Balmer decrement (i.e. $D_{34}$ and
$D_{54}$) values in classical Be stars. Subsequently, we estimated the Balmer
decrement values for 105 program stars and found that $\approx$ 20\% of them
show $D_{34}$ $\geq$ 2.7, implying that their circumstellar disc are generally
optically thick in nature. One program star, HD 60855 shows H$\alpha$ in
absorption -- indicative of discless phase. From our analysis, we found that in
classical Be stars, H$\alpha$ emission equivalent width values are mostly lower
than 40 \AA, which agrees with that present in literature. Moreover, we noticed
that a threshold value of $\sim$ 10 \AA~of H$\alpha$ emission equivalent width
is necessary for Fe{\sc ii} emission to become visible. We also observed that
emission line equivalent widths of H$\alpha$, P14, Fe{\sc ii} 5169 and O{\sc i}
8446 \AA~for our program stars tend to be more intense in earlier spectral
types, peaking mostly near B1-B2. Furthermore, we explored various formation
regions of Ca{\sc ii} emission lines around the circumstellar disc of classical
Be stars. We suggest the possibility that Ca{\sc ii} triplet emission can
originate either in the circumbinary disc or from the cooler outer regions of
the disc, which might not be isothermal in nature.
