  We present the analysis of four M dwarf stars -plus one M giant that seeped
past our selection criteria- observed in Cycle 3 of Kepler Guest Observer
program (GO3) in a search for intrinsic pulsations. Stellar oscillations in M
dwarfs were theoretically predicted by Rodr\'iguez-L\'opez et al. (2012) to be
in the range ~20-40 min and ~4-8 h, depending on the age and the excitation
mechanism. We requested Kepler short cadence observations to have an adequate
sampling of the oscillations. The targets were chosen on the basis of
detectable rotation in the initial Kepler results, biasing towards youth.The
analysis reveals no oscillations attributable to pulsations at a detection
limit of several parts per million, showing that either the driving mechanisms
are not efficient in developing the oscillations to observable amplitudes, or
that if pulsations are driven, the amplitudes are very low. The size of the
sample, and the possibility that the instability strip is not pure, allowing
the coexistence of pulsators and non-pulsators, prevent us from deriving
definite conclusions. Inmediate plans include more M dwarfs photometric
observations of similar precision with Kepler K2 mission and spectroscopic
searches already underway within the Cool Tiny Beats Project (Anglada-Escud\'e
et al. 2014, Berdi\~nas et al. 2014) with the high-resolution spectrographs
HARPS and HARPS-N.
