  We have performed detailed high-resolution spectroscopic analysis on seven
metal-poor stars (BD+75 348, BD+09 3019, HD238020, HE0319-0215, HE0507-1653,
HE0930-0018, HE1023-1504) and derived their atmospheric parameters T$_{eff}$,
log$g$, [Fe/H], and mictroturbulent velocity ($\xi$). The metallicity range is
found to be -2.57$<$[Fe/H]$<$-0.42. The elemental abundances of 17 light
elements and 12 heavy elements are estimated. We have classified BD+75 348 and
BD+09 3019 as strong Ba stars, HD238020 as a mild Ba star, and the remaining
four objects as CEMP-s stars. We have estimated the masses of the stars from
Hertzsprung-Russel (HR) diagram, and, compiling the data of 205 Ba stars from
literature, estimated the mass distribution of Ba stars. We have also estimated
the initial masses of the companion AGBs of the program stars as well as the
masses of the companion AGBs of 159 Ba and 36 CEMP-s stars from literature,
with the help of a parametric-model-based analysis using FRUITY models. While
the primary mass distribution of mild Ba stars peaks at 3.7 M$_{\odot}$, for
the strong Ba stars the peak appears at 2.5 M$_{\odot}$. We, therefore, propose
that the initial masses of the progenitor AGBs dominantly control the formation
of mild and strong Ba stars. However, a clear overlap, in the range 1.3-4.0
M$_{\odot}$, noticed between the progenitor masses of both the subclasses of Ba
stars, may indicate that other factors, such as metallicities and the orbital
periods, may also have significant contributions. The progenitor AGBs' mass
distribution of CEMP-s stars is found to peak at 2.03 M$_{\odot}$.
