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We present the results of a multiplicity survey of 212 T Tauri stars in theChamaeleon I and Taurus-Auriga star-forming regions, based on high-resolutionspectra from the Magellan Clay 6.5 m telescope. From these data, we achieved atypical radial velocity precision of ~80 m/s with slower rotators yieldingbetter precision, in general. For 174 of these stars, we obtained multi-epochdata with sufficient time baselines to identify binaries based on radialvelocity variations. We identified eight close binaries and four close triples,of which three and two, respectively, are new discoveries. The spectroscopicmultiplicity fractions we find for Cha I (7%) and Tau-Aur (6%) are similar toeach other, and to the results of field star surveys in the same mass andperiod regime. However, unlike the results from imaging surveys, the frequencyof systems with close companions in our sample is not seen to depend on primarymass. Additionally, we do not find a strong correlation between accretion andclose multiplicity. This implies that close companions are not likely the mainsource of the accretion shut down observed in weak-lined T Tauri stars. Ourresults also suggest that sufficient radial velocity precision can be achievedfor at least a subset of slowly rotating young stars to search for hot Jupiterplanets.

Close Companions to Young Stars. I. A Large Spectroscopic Survey in Chamaeleon I and Taurus-Auriga