  The discovery that Vega is a rapidly rotating pole-on star has raised a
number of questions about this fundamental standard, including such issues as
its composition, and in turn its mass and age. We report here a reanalysis of
Vega's composition. A full spectral synthesis based on the Roche model derived
earlier from NPOI interferometry is used. We find the line shapes in Vega's
spectrum to be more complex than just flat-bottomed, which have been previously
reported; profiles range from slightly self-reversed to simple ``V'' shapes. A
high SNR spectrum, obtained by stacking spectra from the ELODIE archive, shows
excellent agreement with the calculations, provided we add about 10 km/s of
macroturbulence to the predicted spectra. From the abundance analysis, we find
that Vega shows the peculiar abundance pattern of a \W Bootis star as
previously suggested. We investigate the effects of rotation on the deduced
abundances and show that the dominant ionization states are only slightly
affected compared to analyses using non-rotating models. We argue that the
rapid rotation requires the star be fully mixed. The composition leads to
masses and particularly ages that are quite different compared to what are
usually assumed.
