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Dominated by a single, large‐amplitude pulsation mode, the rapidly pulsating hot subdwarf B star CS 1246 is a prime candidate for a long‐term O−C diagram study. We collected nearly 400 h of photometry with the 0.41‐m Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes over a time‐span of 14 months to begin looking for secular variations in the pulse timings. Interestingly, the O−C diagram is dominated by a strong sinusoidal pattern with a period of 14.1 d and an amplitude of 10.7 light‐seconds. Underneath this sine wave is a secular trend implying a decrease in the 371.7‐s pulsational period of , which we attribute to the evolution of the star through the Hertzsprung–Russell diagram. The sinusoidal variation could be produced by the presence of a low‐mass companion, with  m  sin  i ≃ 0.12 M ⊙ , orbiting the subdwarf B star at a distance of 20 R ⊙ . An analysis of the combined light curve reveals the presence of a low‐amplitude first harmonic to the main pulsation mode.

Fortnightly fluctuations in the O−C diagram of CS 1246 ★