Carbon-enhanced metal-poor ( CEMP ) stars bear important imprints of the early chemical enrichment of any stellar system .
While these stars are known to exist in copious amounts in the Milky Way halo , detailed chemical abundance data from the faint dwarf spheroidal ( dSph ) satellites are still sparse , although the relative fraction of these stars increases with decreasing metallicity .
Here , we report the abundance analysis of a metal-poor ( [ Fe/H ] = -2.5 dex ) , carbon-rich ( [ C/Fe ] =1.4 dex ) star , ALW-8 , in the Carina dSph using high-resolution spectroscopy obtained with the ESO/UVES instrument .
Its spectrum does not indicate any over-enhancements of neutron capture elements .
Thus classified as a CEMP-no star , this is the first detection of this kind of star in Carina .
Another of our sample stars , ALW-1 , is shown to be a CEMP- s star , but its immediate binarity prompted us to discard it from a detailed analysis .
The majority of the 18 chemical elements we measured are typical of Carina ’ s field star population and also agree with CEMP stars in other dSph galaxies .
Similar to the only known CEMP-no star in the Sculptor dSph and the weak- r -process star HD 122563 , the lack of any strong barium-enhancement is accompanied by a moderate overabundance in yttrium , indicating a weak r -process activity .
The overall abundance pattern confirms that , also in Carina , the formation site for CEMP-no stars has been affected by both faint supernovae and by standard core collapse supernovae .
Whichever process was responsible for the heavy element production in ALW-8 must be a ubiquitous source to pollute the CEMP-no stars , acting independently of the environment such as in the Galactic halo or in dSphs .