The Bar in NGC 936

The light from the SBO galaxy is decomposed into three components: an oblate spheroidal bulge with luminosity 5.8 x 10^9^ L_sun_ and true ellipticity ɛ = 0.63, a rectangular bar with luminosity 5.6 x 10^9^ L_sun_ and size 8.0 x 2.2 kpc, and a constant-intensity lens with luminosity 5.6 x 10^9^ L_sun_ out to 6.4 kpc. The bulge radial-luminosity profile is best described by a truncated King model approximation rather than a De Vaucouleurs law. The azimuthally averaged bar and lens form an exponential profile with scale length 3.5 kpc. The dynamics are explored in detail. A brief survey of orbits is made assuming that the mass/light ratio is constant. For any reasonable pattern speed of the bar an inner Lindblad resonance always exists. Stable bar-forming x_1_ orbits exist out to a radius of at least 4 kpc along the bar major axis provided that the co-rotation radius (more specifically, the radius of the Lagrange points L_1_ and L_2_) is greater than about 5.0 kpc. An approximate dynamical model is constructed by taking the bulge to be an oblare isotropic rotator and by scaling the predicted disk kinematics from an n-body simulation of Sparke and Sellwood. The stellar rotation curve along the bar should show a nearly constant angular rotation rate slightly higher than the pattern speed. Very high streaming motions should exist along the bar minor axis. Existing observations are consistent with the former prediction but not the latter; however, along the minor axis, the bulge light overwhelms the bar light and may mask the streaming motions.