Abstract

The ability to trace stars to common progenitors by using chemical abundance patterns (i.e. chemical tagging) is an integral component of Galactic Archeology. Determining to what extent we are able to believe conatal stars are chemically identical is critical to the feasibility of this method. We present detailed chemical abundances of 35 comoving pairs. Many of these pairs were likely conatal stars. These stars were selected specifically

to have similar stellar parameters in order to reduce the influence of systematic errors in the abundance analysis. We measure abundances for 24 elements including Li, C, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, Y, Zr, Ba, La, Nd, Eu. We build upon previous studies of very wide binaries and co-moving pairs by examining systems with separations up to 100 pc. We find several comoving pairs between 20 and 60 parsecs which have metallicity differences below 0.05 dex. We find no significant increase in the spread of the metallicity difference as a function of separation.