Abstract
A faint (V = 13.11, B-V = -0.15) high altitude (b = +640) star discovered by G. Haro to have Hα in emission is of type BO-B 1, and has the appearance of a typical Population I Be star. If that were so, there would be difficulty in accounting for the star's presence at z = 19.7 kpc if it were formed near the plane no more than 1-2 x 10 years ago. The Balmer absorption wings, outside the emission cores, make possible an estimate of log g by comparison with other early B-type stars of various luminosities; the result is log g is about 4.7, which shows that Haro's star lies below the main-sequence. If it is a Population II star with mass about 0.6 Me, then Mv is about +2, and the distance is only 1.6 kpc. Possibly Haro's star is in transition between the AGB and planetary nebula central star stages. A search of globular clusters for similar objects is recommended.
