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We examine the relation between stellar mass and central stellar velocitydispersion-the M-sigma relation-for massive quiescent galaxies at z<0.7. Wemeasure the local relation from the Sloan Digital Sky Survey and theintermediate redshift relation from the Smithsonian Hectospec Lensing Survey.Both samples are highly complete (>85%) and we consistently measure the stellarmass and velocity dispersion for the two samples. The M-sigma relation and itsscatter are independent of redshift with sigma ~ M^0.3 for M>10^10.3 M_solar.The measured slope of the M-sigma relation is the same as the scaling betweenthe total halo mass and the dark matter halo velocity dispersion obtained byN-body simulations. This consistency suggests that massive quiescent galaxiesare virialized systems where the central dark matter concentration is either aconstant or negligible fraction of the stellar mass. The relation between thetotal galaxy mass (stellar + dark matter) and the central stellar velocitydispersion is consistent with the observed relation between the total mass of agalaxy cluster and the velocity dispersion of the cluster members. This resultsuggests that the central stellar velocity dispersion is directly proportionalto the velocity dispersion of the dark matter halo. Thus the central stellarvelocity dispersion is a fundamental, directly observable property of galaxiesthat may robustly connect galaxies to dark matter halos in N-body simulations.To interpret the results further in the context of Lambda-CDM, it would beuseful to analyze the relationship between the velocity dispersion of stellarparticles and the velocity dispersion characterizing their dark matter halos inhigh-resolution cosmological hydrodynamic simulations.

The Scaling of Stellar Mass and Central Stellar Velocity Dispersion for Quiescent galaxies at z < 0.7