High chemical abundances in H I deficient spirals of the virgo cluster

New spectroscopic observations of H II regions, together with published data, are used to derive interstellar O abundances in 9 late-type spiral galaxies in the Virgo cluster. The galaxies are divided into 3 groups according to their deficiency of H I relative to normal field spirals. Generally, the most H I deficient galaxies are closest to the cluster core. The outlying spirals with normal H I content show abundances and radial abundance gradients similar to those in field spirals. The H I deficient galaxies show abundances larger by about 0.3 dex and relatively flat radial gradients. The galaxies with an intermediate degree of H I deficiency are intermediate in O abundance. These results confirm and clarify earlier indications that spirals evolve to higher chemical abundances in the cluster environment. Simple chemical evolution models indicate that curtailment of infall into spirals in the cluster core may explain part of the abundance differential, but there appears to be a need for other mechanisms.