We explore the possible connection between the open cluster IC 2391 and the unbound Argus association identified by the SACY survey .
In addition to common kinematics and ages between these two systems , here we explore their chemical abundance patterns to confirm if the two substructures shared a common origin .
We carry out a homogenous high-resolution elemental abundance study of eight confirmed members of IC 2391 as well as six members of the Argus association using UVES spectra .
We derive spectroscopic stellar parameters and abundances for Fe , Na , Mg , Al , Si , Ca , Ti , Cr , Ni and Ba .

All stars in the open cluster and Argus association were found to share similar abundances with the scatter well within the uncertainties , where [ Fe/H ] = - 0.04 \pm 0.03 for cluster stars and [ Fe/H ] = - 0.06 \pm 0.05 for Argus stars .
Effects of over-ionisation/excitation were seen for stars cooler than roughly 5200 K as previously noted in the literature .
Also , enhanced Ba abundances of around 0.6 dex were observed in both systems .
The common ages , kinematics and chemical abundances strongly support that the Argus association stars originated from the open cluster IC 2391 .
Simple modeling of this system find this dissolution to be consistent with two-body interactions .