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Carbon-enhanced metal-poor (CEMP) stars span a wide range of stellarpopulations, from bona fide second-generation stars to later forming stars thatprovide excellent probes of, e.g., binary mass transfer. Here we analyse 11metal-poor stars of which 10 are CEMP stars. Based on high signal-to-noise(SNR) X-Shooter spectra, we derive abundances of 20 elements (C, N, O, Na, Mg,Ca, Sc, Ti, Cr, Mn, Fe, Ni, Sr, Y, Ba, La, Ce, Pr, Nd, Eu). From the high SNRspectra, we trace the chemical contribution of the rare earth elements (REE)from various production sites, finding a preference for metal-poor low-mass AGBstars of 1.5Mo in CEMP-s stars, while CEMP-r/s stars may indicate a moremassive AGB contribution (2-5Mo). A contribution from the r-process - possiblyfrom neutron star mergers (NSM), is also detectable in the REE abundances,especially in the CEMP-r/s. Combining spectra with Gaia DR2 astrometric dataindicates that all but one star in our sample (and most literature stars)belong to the Galactic halo. They exhibit a median orbital eccentricity of 0.7,and are found on both pro- and retrograde orbits. The orbital parameters ofCEMP-no and CEMP4s stars are remarkably similar in the 98 stars we study. Aspecial CEMP-no star, with very low Sr and Ba content, possesses the mosteccentric orbit among the stars in our sample, passing close to the Galacticcentre. Finally, we propose an improved scheme to sub-classify the CEMP stars,making use of the Sr$/$Ba ratio, which can also be used to separate verymetal-poor stars from CEMP stars in 93 stars in the metallicity range$-4.2<$[Fe/H]$<-2$. The Sr/Ba ratio can also be used for distinguishingCEMP-s,-r/s and -no stars. The Sr/Ba ratio is also a powerful astro-nuclearindicator, as AGB stars exhibit very different Sr/Ba ratios, compared to fastrotating massive stars and NSM, and it is fairly unbiased by NLTE and 3Dcorrections.(abridged)

Abundances and kinematics of carbon-enhanced metal-poor stars in the Galactic halo*; A new classification scheme based on Sr and Ba