v 1 8 M ay 2 00 3 Possible Post - AGB Stars

Radial velocities were measured for 5 potential post-AGB stars, two in the globular cluster NGC 1851 and three in the dSph galaxy Ursa Minor. All five potential PAGB stars were found to be radial velocity non-members. Eskridge & Schweitzer 2001 reported proper motion memberships for 3 stars that fall in the post-AGB region of the CM diagram of the UMi system. In 2003 we obtained spectra during heavily overcast full moon engineering time at the Hobby-Eberly Telescope (HET) with the High Resolution Spectrograph (HRS, Tull et al. 1998). The spectra were taken in the lowest resolution mode (R = 15, 000) and had signal-to-noise ratios between 10 and 20 per resolution element. The spectra where reduced with IRAF 2 echelle scripts. The velocities for the three Ursa Minor stars are given in Table 1. Since the velocity of the UMi galaxy is known to be-248 km/sec, it appears that these stars are not members. In addition in 1997 the authors obtained 4-m echelle spectra of 2 likely post-AGB stars in the globular cluster NGC 1851, stars W266 and W464 (Walker 1992). Both stars showed velocities near zero and hence are very likely to also be non-members of NGC 1851.