TY - JOUR
T1 - Search for associations containing young stars
T2 - chemical tagging IC 2391 and the Argus association
AU - De Silva, G. M.
AU - D'Orazi, V.
AU - Melo, C.
AU - Torres, C. A O
AU - Gieles, M.
AU - Quast, G. R.
AU - Sterzik, M.
N1 - This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. Copyright 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
PY - 2013
Y1 - 2013
N2 - We explore the possible connection between the open cluster IC 2391 and the unbound Argus association identified by the search for associations containing young stars 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 ± 0.03 for cluster stars and [Fe/H] = -0.06 ± 0.05 for Argus stars. Effects of overionization/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 the fact that the Argus association stars originated from the open cluster IC 2391. Simple modelling of this system finds this dissolution to be consistent with two-body interactions.
AB - We explore the possible connection between the open cluster IC 2391 and the unbound Argus association identified by the search for associations containing young stars 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 ± 0.03 for cluster stars and [Fe/H] = -0.06 ± 0.05 for Argus stars. Effects of overionization/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 the fact that the Argus association stars originated from the open cluster IC 2391. Simple modelling of this system finds this dissolution to be consistent with two-body interactions.
UR - http://www.scopus.com/inward/record.url?scp=84876831251&partnerID=8YFLogxK
U2 - 10.1093/mnras/stt153
DO - 10.1093/mnras/stt153
M3 - Article
AN - SCOPUS:84876831251
SN - 0035-8711
VL - 431
SP - 1005
EP - 1018
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -