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We present the analysis of four M dwarf stars -plus one M giant that seepedpast our selection criteria- observed in Cycle 3 of Kepler Guest Observerprogram (GO3) in a search for intrinsic pulsations. Stellar oscillations in Mdwarfs were theoretically predicted by Rodr\'iguez-L\'opez et al. (2012) to bein the range ~20-40 min and ~4-8 h, depending on the age and the excitationmechanism. We requested Kepler short cadence observations to have an adequatesampling of the oscillations. The targets were chosen on the basis ofdetectable rotation in the initial Kepler results, biasing towards youth.Theanalysis reveals no oscillations attributable to pulsations at a detectionlimit of several parts per million, showing that either the driving mechanismsare not efficient in developing the oscillations to observable amplitudes, orthat if pulsations are driven, the amplitudes are very low. The size of thesample, and the possibility that the instability strip is not pure, allowingthe coexistence of pulsators and non-pulsators, prevent us from derivingdefinite conclusions. Inmediate plans include more M dwarfs photometricobservations of similar precision with Kepler K2 mission and spectroscopicsearches already underway within the Cool Tiny Beats Project (Anglada-Escud\'eet al. 2014, Berdi\~nas et al. 2014) with the high-resolution spectrographsHARPS and HARPS-N.

M dwarf search for pulsations within Kepler GO program