Despite their diminutive stature, M dwarfs are ideal targets for exoplanet searches. Seventy-five percent of stars in the galaxy are M dwarfs and the Kepler mission revealed that planetary systems orbiting small stars are enticingly common: the typical early M dwarf hosts 2.5 planets smaller than Neptune with periods shorter than 200 days and one in four early M dwarfs harbors a potentially habitable planet. More recently, the discoveries of several potentially habitable planets orbiting late M dwarfs may indicate that the smallest stars host habitable planets at an even higher frequency than larger M dwarfs. In addition to their prevalence and their high rate of planet occurrence, M dwarfs are attractive targets for exoplanet studies because planets orbiting small stars are more detectable: for a planet with a fixed size and insolation flux, transits will be deeper, more frequent, and more likely to occur if the planet orbits a smaller star. Similarly, a planet with a fixed mass induces a larger radial velocity signal when orbiting a low-mass star. Despite the small physical size of the habitable zones of M dwarfs, many of these stars are close enough that planets within their habitable zones could be directly imaged by the next generation of extremely large telescopes. Recognizing this “M Dwarf Advantage,” a slew of ground-based facilities specifically designed to detect planets orbiting M dwarfs have already begun operations and many more are preparing to start searching for planets orbiting the nearest stars. I will review past discoveries about the treasure trove of planets orbiting M dwarfs and discuss upcoming plans to detect even more planets orbiting these red gems. In particular, I will highlight the NASA TESS mission and the prospects for detecting hundreds of transiting planets orbiting the brightest and nearest M dwarfs. These planets will be extremely attractive targets for radial velocity mass measurement with red spectrographs and atmospheric characterization with *Spitzer*, *HST* and *JWST*.