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We are carrying out a large ancillary program with the SDSS-III, using thefiber-fed multi-object NIR APOGEE spectrograph, to obtain high-resolutionH-band spectra of more than 1200 M dwarfs. These observations are used tomeasure spectroscopic rotational velocities, radial velocities, physicalstellar parameters, and variability of the target stars. Here, we describe thetarget selection for this survey and results from the first year of scientificobservations based on spectra that is publicly available in the SDSS-III DR10data release. As part of this paper we present RVs and vsini of over 200 Mdwarfs, with a vsini precision of ~2 km/s and a measurement floor at vsini = 4km/s. This survey significantly increases the number of M dwarfs studied forvsini and RV variability (at ~100-200 m/s), and will advance the targetselection for planned RV and photometric searches for low mass exoplanetsaround M dwarfs, such as HPF, CARMENES, and TESS. Multiple epochs of radialvelocity observations enable us to identify short period binaries, and AOimaging of a subset of stars enables the detection of possible stellarcompanions at larger separations. The high-resolution H-band APOGEE spectraprovide the opportunity to measure physical stellar parameters such aseffective temperatures and metallicities for many of these stars. At theculmination of this survey, we will have obtained multi-epoch spectra and RVsfor over 1400 stars spanning spectral types of M0-L0, providing the largest setof NIR M dwarf spectra at high resolution, and more than doubling the number ofknown spectroscopic vsini values for M dwarfs. Furthermore, by modelingtelluric lines to correct for small instrumental radial velocity shifts, wehope to achieve a relative velocity precision floor of 50 m/s for bright Mdwarfs. We present preliminary results of this telluric modeling technique inthis paper.

The SDSS-III APOGEE Radial Velocity Survey of M dwarfs I: Description of Survey and Science Goals