We present results from 1351 high resolution spectra of 1215 stars in the Orion Nebula Cluster ( ONC ) and the surrounding Orion 1c association , obtained with the Hectochelle multiobject echelle spectrograph on the 6.5m MMT .
We confirmed 1111 stars as members , based on their radial velocity and/or H \alpha  emission .
The radial velocity distribution of members shows a dispersion of \sigma = 3.1 km s ^ { -1 } .
We found a substantial north-south velocity gradient and spatially coherent structure in the radial velocity distribution , similar to that seen in the molecular gas in the region .
We also identified several binary and high velocity stars , a region exhibiting signs of triggered star formation , and a possible foreground population of stars somewhat older than the ONC .
Stars without infrared excesses ( as detected with the IRAC instrument on the Spitzer Space Telescope ) exhibit a wider spread in radial velocity than the infrared excess stars ; this spread is mostly due to a blue-shifted population of stars that may constitute a foreground population .
We also identify some accreting stars , based on H \alpha , that do not have detectable infrared excesses with IRAC , and thus are potential transitional disk systems ( objects with inner disk holes ) .
We propose that the substructure seen both in stellar and gaseous component is the result of non-uniform gravitational collapse to a filamentary distribution of gas .
The spatial and kinematic correlation between the stellar and gaseous components suggests the region is very young , probably only \sim 1 crossing time old or less to avoid shock dissipation and gravitational interactions which would tend to destroy the correlation between stars and gas .