UMa Moving Group chronochemokinematic analysis

We determine the most likely metallicity for the unevolved stars of the group, collectively, by assuming that these stars all conform to a single zero-age main sequence line and requiring that residual T_eff_ and luminosity values be minimized: the [Fe/H] value that best describes the observed HR diagram of the group lies in the range +0.05<[Fe/H]<+0.10.

In this work, we report the detailed spectroscopic analysis of 23 stars in the Ursa Major Group (UMaG), together with seven young field stars that function as a control sample, based on high S/N, R~60000 optical spectra. We present abundances for C, Na, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Fe, Ni, Cu, Zn, Sr, Y, Zr, Ba, La, Ce, Nd, Sm, Gd, and Eu. We also found that there is a clear kinematic nucleus in the UVW space, but from the spectroscopic analysis only a fraction of these stars could be considered chemically and chronologically homogeneous.