2011ApJ...739L..47B

We measure the contribution of galaxy disks to the overall gravitational potential of 30 nearly face-on intermediate-to-late-type spirals from the DiskMass Survey. The central vertical velocity dispersion of the disk stars (σ^disk_z, R = 0_) is related to the maximum rotation speed (V_max) as σ^disk_z, R = 0_∼ 0.26V_max, consistent with previous measurements for edge-on disk galaxies and a mean stellar velocity ellipsoid axial ratio α ≡ σ_z/σ_R= 0.6. For reasonable values of disk oblateness, this relation implies these galaxy disks are submaximal. We find disks in our sample contribute only 15%-30% of the dynamical mass within 2.2 disk scale lengths (h_R), with percentages increasing systematically with luminosity, rotation speed, and redder color. These trends indicate that the mass ratio of disk-to-total matter remains at or below 50% at 2.2 h_R even for the most extreme, fast-rotating disks (V_max ≥ 300 km/s) of the reddest rest frame, face-on color (B - K ∼ 4 mag), and highest luminosity (M_K< -26.5 mag). Therefore, spiral disks in general should be submaximal. Our results imply that the stellar mass-to-light ratio and hence the accounting of baryons in stars should be lowered by at least a factor of three.