Data from the VVV NIR survey of the inner Milky Way show that our Galaxy has a strongly peanut-shaped bulge. Extending the analysis to larger radii with other surveys shows that the long bar is aligned with the bulge out to about 20 degrees longitude, followed by a region of transition to the Galactic disk. Dynamical models based on the 3D bulge density and the BRAVA kinematic data allow us to determine the mass in the bulge region and to put constraints on the mass-to-light ratio and IMF of the bulge stars as well as on the bar's pattern speed.