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WC 11 stars are a class of cool, subluminous WR stars which are characterized by strong carbon emission lines along with Balmer and forbidden lines from very compact, low-excitation planetary nebulas surrounding the star. It is still a puzzle what stage they represent in the evolution of the star. It has been suggested that they are approaching the AGB for the second time after undergoing a ``last thermal pulse". Alternatively it has been suggested that they are protoplanetary nebulae. Possibly they form a link between planetary nebulae and RCrB stars. Past IUE observations of three other known WC 11 stars have revealed peculiar abundance features and peculiarities in the reddening properties of the surrounding dust. I report on recent IUE observations of a fourth member of this class, IRAS 17514-1555.
