  The Carbon-Enhanced Metal-Poor (CEMP) stars with no enhancement of
neutron-capture elements, the so-called CEMP-no stars are believed to be the
direct descendants of first-generation stars and provide a unique opportunity
to probe the early Galactic nucleosynthesis. We present a detailed chemical and
kinematic analysis for two extremely metal-poor stars HE1243$-$2408 and
HE0038$-$0345 using high-resolution (R${\sim}$86,000) HERMES spectra. For the
object HE1243$-$2408, we could make a detailed comparison with the available
literature values; however, only limited information is available for the other
object HE0038$-$0345. Our estimated metallicity for these two objects are
$-$3.05 and $-$2.92 respectively. With estimated [C/Fe] (1.03 and 1.05) and
[Ba/Fe] ($-$0.18 and $-$0.11) respectively, the objects are found to be
bonafide CEMP-no stars. From the observed abundances of C, Na, Mg, and Ba
(i.e., A(C), A(Na), A(Mg), A(Ba)), the objects are found to belong to Group II
CEMP-no stars. A detailed abundance profile analysis indicates that the objects
are accreted from dSph satellite galaxies that support hierarchical Galaxy
assembly. Further, our analysis shows that the progenitors of the stars are
likely Pop II Core-Collapse Supernovae. The object HE0038$-$0345 is found to be
a high-energy, prograde, outer-halo object, and HE1243$-$2408 is found to be a
high-energy, retrograde, inner-halo object. Our detailed chemodynamical
analysis shows that HE1243$-$2408 is related to I'itoi structure, where as
HE0038$-$0345 is likely related to Sgr or GSE events. The mass of the
progenitor galaxies of the program stars inferred from their dynamics is at par
with their likely origin in massive dSph galaxies.
