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About half of the hot subdwarfs are found to have spectra of composite types,indicating a main sequence companion of spectral type F-K, and the pulsatorsare no exception to this rule. The spectroscopic contamination from the mainsequence stars makes it hard to reliably establish physical parameters for thehot component, and also makes pulsations harder to detect as the amplitudes aredepressed. The binary fraction of the observed sample of hot subdwarf pulsatorsis discussed, as are the biases that are affecting it. Spectroscopic evidenceis presented that clearly demonstrates that the well known sdB pulsator,EOCeti, is misclassified, and is actually an sdOV star.

Pulsating hot subdwarfs with MS companions or: EO Ceti is an sdO pulsator!