  We present a comprehensive analysis of the detailed chemical abundances for a
sample of 11 metal-poor, very metal-poor and extremely metal-poor stars ([Fe/H]
= -1.65 to [Fe/H] = -3.0) as part of the HESP-GOMPA (Galactic survey Of Metal
Poor stArs) survey. The abundance determinations encompass a range of elements,
including C, Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, and
Ba, with a subset of the brighter objects allowing for the measurement of
additional key elements. Notably, the abundance analysis of a relatively bright
highly r-process-enhanced (r-II) star (SDSS J0019+3141) exhibits a
predominantly main r-process signature and variations in the lighter r-process
elements. Moreover, successful measurements of thorium in this star facilitate
stellar age determinations. We find a consistent odd-even nucleosynthesis
pattern in these stars, aligning with expectations for their respective
metallicity levels, thus implicating Type II supernovae as potential
progenitors. From the interplay between the light and heavy r-process elements,
we infer a diminishing relative production of light r-process elements with
increasing Type II supernova contributions, challenging the notion that Type II
supernovae are the primary source of these light r-process elements in the
early Milky Way. A chemodynamical analysis based on Gaia astrometric data and
our derived abundances indicates that all but one of our program stars are
likely to be of accreted origin. Additionally, our examination of alpha-poor
stars underscores the occurrence of an early accretion event from a satellite
on a prograde orbit, similar to that of the Galactic disc.
