It is interesting to compare this model with other bar models proposed for the Milky Way. The position angle of the bar major axis to the viewing direction is close to the suggested by Weinberg (1992), but is considerably larger than the favoured by Binney et al. (1991). On the other hand, the pattern speed of the bar in the simulation places co-rotation at about 2.6 kpc, in good agreement with the 2.4 kpc favoured by Binney et al., but the semi-major axis is considerably less than Weinberg's estimate of 5 kpc. Blitz & Spergel (1991 and this meeting), from an analysis of the balloon borne near IR surface photometry, claim to see a short bar at a still larger angle, but again in the same quadrant. Whitelock (1992) finds a longitudinal asymmetry in the distribution of IRAS selected Mira variables, which she also attributes to a bar. All these strands of evidence indicate a bar-like feature pointing in a similar direction and the case for the COBE ``bulge'' feature being a bar now appears quite strong.