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Cool main-sequence, sub-giant and red-giant stars all show solar-likeoscillations, pulsations that are excited and intrinsically damped bynear-surface convection. Many overtones are typically excited to observableamplitudes, giving a rich spectrum of detectable modes. These modes provide awealth of information on fundamental stellar properties. However, the radialvelocity shifts induced by these oscillations can also be problematic whensearching for low-mass, long-period planets; this is because their amplitudesare large enough to completely mask such minute planetary signals. Here we showhow fine-tuning exposure times to the stellar parameters can help efficientlyaverage out the solar-like-oscillation-induced shifts. To reduce theoscillation signal to the radial velocity precision commensurate with anEarth-analogue, we find that for cool, low-mass stars (near spectral type K)the necessary exposure times may be as short as 4 minutes, while for hotter,higher-mass stars (near spectral type F, or slightly evolved) the requiredexposure times can be longer than 100 minutes. We provide guideline exposuredurations required to suppress the total observed amplitude due to oscillationsto a level of $0.1\,\rm m\,s^{-1}$, and a level corresponding to theEarth-analogue reflex amplitude for the star. Owing to the intrinsic stochasticvariability of the oscillations, we recommend in practice choosing shortexposure durations at the telescope and then averaging over those exposureslater, as guided by our predictions. To summarize, as we enter an era of$0.1\,\rm m\,s^{-1}$ instrumental precision, it is critical to tailor ourobserving strategies to the stellar properties.

Filtering solar-like oscillations for exoplanet detection in radial velocity observations