The Figure illustrates the parallactic motion of Teegarden's Star (Teegarden et al. 2003, Discovery of a New Nearby Star, ApJ 589, L51). The technique illustrated in the Figure is common for initial estimates of a stellar parallax (eg.Gatewood et al. 1985, Short-Interval Estimations of Trigonometric Parallaxes, PASP 97, 345). The proper motion of the star is listed in the USNO B1.0 catalog (Monet, et al. 2003, http://www.nofs.navy.mil/data/fchpix/) as +3436 +/- 2 and -3810 +/- 3 mas per year in RA and Dec. respectively. As a check of the motion and our reduction to the B1.0 catalog, we included the 1951 Palomar position in our analysis of the relative parallax, J2000 position, and proper motion. We find: RA mu RA Dec mu Dec parallax h m s s/yr o ' " "/yr " 2 53 00.867 +0.239273 16 52 52.90 -3.81014 +0.2574 +/- 0.0001 .000011 0.001 0.00015 0.0023 where all of the errors are strictly internal and do not reflect the uncertainties in the reference system or the adjustment of the relative parallax to absolute. An estimate of the reduction to absolute is difficult at this stage, but we note that all of the reference star proper motions are small and that their average apparent visual magnitude is approximately 16. Adopting a parallax of 0.259 +/- 0.004 gives a distance of 3.86 +/- 0.06 parsecs and distance modulus of 2.067 +/- 0.034 magnitudes. Thus our initial analysis indicates that this M6.5 star has an absolute visual magnitude of 17.47 +/- 0.04.
Our findings are in excellent agreement with those of the US Naval Observatory (Conrad Dahn, private communications).