THE ASTRONOMICAL JOURNAL    VOLUME 113, NUMBER 1, PAGE 321     JANUARY 1997

          A NEW SURVEY OF STELLAR KINEMATICS IN THE CENTRAL MILKY WAY

                       GLENN P. TIEDE AND D. M. TERNDRUP

     Department of Astronomy, The Ohio State University, 174 W. 18th Ave.,
                             Columbus, Ohio 43210

    We present the results of a photometric and spectroscopic study of 189
    stars in a field at (l,b)=(8.4 deg,-6.0 deg). We measure radial
    velocities and selected indices of line strength from the spectra and
    derive reddening, metallicity, photometric parallaxes, and azimuthal
    rotation velocities and dispersion. We find an average reddening and
    extinction to the field of E(V-I)=0.43+/-0.09 and A_V=1.07+/-0.22. We
    use distances derived from photometric parallaxes and find that the
    distribution of stars along this line of sight is not strongly peaked
    at the tangent point. In an attempt to understand the apparent decrease
    in line-of-sight velocity dispersion with increasing metallicity, we
    divide our sample into metal-rich and metal-poor groups. Though we lack
    enough stars to statistically analyze each group, we find the average
    distances of the metal-rich and metal-poor groups to be, <R>=3.1 kpc
    and <R>=7.0 kpc. Excluding stars in our sample which are likely to be
    in the foreground disk, we calculate a rotational velocity for the
    bulge of Vrot=97+/-9 km/s, sigma_phi=71+/-11 km/s. Combining this
    result with studies at other (l,b), we find a rotation rate for the
    bulge of 10.6+/-0.6 km/s/deg or 77+/-5 km/s/kpc. We conclude that when
    attempting to understand the properties of stars along lines of sight
    into the bulge it is important to consider the line-of-sight
    distribution of the stars, especially when more than a few degrees from
    the galactic center. (Copyright) 1997 American Astronomical Society.