Density of dark matter in the Galactic disk

We determine abundances, luminosities and space motions for a sample of nearby K giants. We analyse their kinematics and argue that we have isolated the local counterpart of the K giants found in a cone at the South Galactic Pole by Bahcall, Flynn & Gould (BFG). For a given description of the vertical potential of the local disc, constructed from the known matter and possible dark matter components, the velocity distribution and space density of these nearby K giants can be calculated as a function of height z above the Galactic plane. Comparison with the BFG observations then allows us to solve for the best-fitting potential. The major result is that the observations can be quite well fitted by the potential due to known matter only. The fit can be improved by invoking dark matter in the disc, but only a small amount is required: if such dark matter is distributed proportionately to the known matter (following Bahcall) our best-fitting model has a disc surface density of o = 52 t 13 M0 , compared to = 49 t 9 M0 for the known disc matter. This determination is in good accord with the Kuijken & Gilmore analysis of disc dark matter from K dwarfs. Key words: celestial mechanics, stellar dynamics - stars: fundamental parameters - stars: giant - Galaxy: kinematics and dynamics - Galaxy: structure - dark matter.