  Observed properties of Wolf-Rayet stars at high metallicity are reviewed.
Wolf-Rayet stars are more common at higher metallicity, as a result of stronger
mass-loss during earlier evolutionary phases with late WC subtypes signatures
of solar metallicity or higher. Similar numbers of early (WC4-7) and late
(WC8-9) stars are observed in the Solar neighbourhood, whilst late subtypes
dominate at higher metallicities, such as Westerlund 1 in the inner Milky Way
and in M83. The observed trend to later WC subtype within metal-rich
environments is intimately linked to a metallicity dependence of WR stars, in
the sense that strong winds preferentially favour late subtypes. This has
relevance to (a) the upper mass limit in metal-rich galaxies such as NGC 3049,
due to softer ionizing fluxes from WR stars at high metallicity; (b)
evolutionary models including a WR metallicity dependence provide a better
match to the observed N(WC)/N(WN) ratio. The latter conclusion partially rests
upon the assumption of constant line luminosities for WR stars, yet
observations and theoretical atmospheric models reveal higher line fluxes at
high metallicity.
