A new kinematic distance estimator to the Large Magellanic Cloud

The distance to the Large Magellanic Cloud (LMC) can be directly determined by measuring three of its properties: its radial velocity field, its mean proper motion, and the position angle phi(ph) of its photometric line of nodes. Statistical errors of similar to 2% are feasible based on proper motions obtained with any of several proposed astrometry satellites, the earliest possibility being the Full-Sky Astrometric Mapping Explorer (FAME). The largest source of systematic error is likely to be in the determination of phi(ph). I suggest two independent methods to measure phi(ph), one based on counts of clump giants and the other on photometry of clump giants. I briefly discuss a variety of methods to test for other sources of systematic errors.