The Galactic halo is thought to form, at least in part, from the accretion of dark-matter dominated mini-halos.  These mini-halos are also responsible for donating the so-called CEMP-no stars to the halo, which are thought to be bona-fide second-generation stars.  A recent study has suggested the existence of multiple pathways to form CEMP-no stars, based on the distinct morphological stellar distribution present in the A(C)-[Fe/H] space. In this talk, I will briefly review our current understanding of the chemodynamical nature of the CEMP-no stars and its implication on the nature of the first stars. I also present important evidence regarding Galactic assembly history revealed by the similarity of CEMP-no group morphology present among the metal-poor stars in satellite dwarf galaxies.