Constraints on galaxy halo profiles from galaxy-galaxy lensing and Tully-Fisher/fundamental plane relations

Abstract

Observations of galaxy-galaxy lensing from Sloan Digital Sky Survey (SDSS) are combined with the Tully-Fisher and fundamental plane relations to derive constraints on galactic halo profiles.We show that both for early and late type galaxies around L* the rotation velocity drops significantly from its peak value at the optical radius to the virial radius, v_opt/v_200 \sim 1.8 with about 20% uncertainty. Such a drop is expected in models in which the halo profile is very concentrated, so that it declines steeper than isothermal at large radii. This large drop can be explained as a result of both a concentrated dark matter profile and a significant stellar contribution to the rotation velocity at the optical radii. We model the stellar component with a thin rotationally supported disk or a Hernquist profile and use adiabatic dark matter response model to place limits on the halo concentration as a function of the stellar mass to light ratio. For reasonable values of the latter we find concentrations consistent with CDM predictions, suggesting there is no evidence for low concentrations for the majority of halos in the universe. We also discuss the origin of Faber-Jackson relation L \propto sigma^4 in light of L \propto v_200^2.5 relation found for early type galaxies from galaxy-galaxy lensing. This leads to a decrease in v_opt/v_{200} with luminosity above L*, so that at 7L_* the ratio is 1.4. This is expected from the fundamental plane relation and implies that relations such as Tully-Fisher and Faber-Jackson are not simply relations between the mass of dark matter halo and galaxy luminosity, but are also significantly influenced by the baryonic effects on the rotation velocity at optical radii.