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We present new time-resolved photometry for two sdB stars, PG 0048+091 and PG 0154+182 , which clearly shows them to be rapidly pulsating stars of the “EC14026” class. In PG 0048+091 we detect, with some confidence, seven frequencies between 5252 and 9368 μHz corresponding to periods between 190 and 107 s. In PG 0154+182 , for which our data are much sparser, we identify only a single frequency near 6090 μHz (164 s). New spectroscopy, combined with archival (2MASS) infrared photometry, indicates that PG 0048+091 has a companion of spectral type near G0V–G2V, whilst PG 0154+182 has a companion of later spectral type, probably in the range G5V–K5V.

The secular evolution of the pulsation period of δ Cephei, η Aquilae, and ζ Geminorum during a cumulative total of 577 years suggests wave-like departures about the smooth time trends.