We have observed 15 red giant stars in the relatively massive , metal-poor globular cluster NGC 4833 using the MIKE spectrograph at Magellan .
We calculate stellar parameters for each star and perform a standard abundance analysis to derive abundances of 43 species of 39 elements , including 20 elements heavier than the iron group .
We derive \langle [ Fe/H ] \rangle = - 2.25 \pm 0.02 from Fe i lines and \langle [ Fe/H ] \rangle = - 2.19 \pm 0.013 from Fe ii lines .
We confirm earlier results that found no internal metallicity spread in NGC 4833 , and there are no significant star-to-star abundance dispersions among any elements in the iron group ( 19 \leq Z \leq 30 ) .
We recover the usual abundance variations among the light elements C , N , O , Na , Mg , Al , and possibly Si .
The heavy-element distribution reflects enrichment by r -process nucleosynthesis ( [ Eu/Fe ] = + 0.36 \pm 0.03 ) , as found in many other metal-poor globular clusters .
We investigate small star-to-star variations found among the neutron-capture elements , and we conclude that these are probably not real variations .
Upper limits on the Th abundance , \log \epsilon ( Th/Eu ) < - 0.47 \pm 0.09 , indicate that NGC 4833 , like other globular clusters where Th has been studied , did not experience a so-called “ actinide boost . ”