Chemical Abundance Analysis of Moving Group W11450 (Latham 1)
  We present elemental abundances for all seven stars in Moving Group W11450
(Latham 1) to determine if they may be chemically related. These stars appear
to be both spatially and kinematically related, but no spectroscopic abundance
analysis exists in literature. Abundances for eight elements were derived via
equivalent width analyses of high resolution (R $\sim$60,000), high
signal-to-noise ratio ($\langle$SNR$\rangle\sim$100) spectra obtained with the
Otto Struve 2.1m telescope and Sandiford Echelle Spectrograph at McDonald
Observatory. The large star-to-star scatter in metallicity, -0.55 $\leq$ [Fe/H]
$\leq$ 0.06 dex ($\sigma$= 0.25), implies these stars were not produced from
the same chemically homogeneous molecular cloud, and are therefore not part of
a remnant or open cluster as previously proposed. Prior to this analysis, it
was suggested that two stars in the group, W11449 & W11450, are possible wide
binaries. The candidate wide binary pair show similar chemical abundance
patterns with not only iron, but with other elements analyzed in this study,
suggesting the proposed connection between these two stars may be real.
