Final results from the Hubble Space Telescope key project to measure the Hubble constant

We present here the final results of the Hubble Space Telescope (HST) Key P roject to measure the Hubble constant. We summarize our method, the results , and the uncertainties, tabulate our revised distances, and give the impli cations of these results for cosmology. Our results are based on a Cepheid calibration of several secondary distance methods applied over the range of about 60-400 Mpc. The analysis presented here benefits from a number of re cent improvements and refinements, including (1) a larger LMC Cepheid sampl e to define the fiducial period-luminosity (PL) relations, (2) a more recen t HST Wide Field and Planetary Camera 2 (WFPC2) photometric calibration, (3 ) a correction for Cepheid metallicity, and (4) a correction for incomplete ness bias in the observed Cepheid PL samples. We adopt a distance modulus t o the LMC (relative to which the more distant galaxies are measured) of mu (o)(LMC) = 18.50 +/- 0.10 mag, or 50 kpc. New, revised distances are given for the 18 spiral galaxies for which Cepheids have been discovered as part of the Key Project, as well as for 13 additional galaxies with published Ce pheid data. The new calibration results in a Cepheid distance to NGC 4258 i n better agreement with the maser distance to this galaxy. Based on these r evised Cepheid distances, we find values (in km s(-1) Mpc(-1)) of H-o = 71 +/- 2 (random) +/- 6 (systematic) (Type Ia supernovae), H-o = 71 +/- 3 +/- 7 (Tully-Fisher relation), H-o = 70 +/- 5 +/- 6 (surface brightness fluctua tions), H-o = 72 +/- 9 +/- 7 (Type II supernovae), and H-o = 82 +/- 6 +/- 9 (fundamental plane). We combine these results for the different methods wi th three different weighting schemes, and find good agreement and consisten cy with H-o = 72 +/- 8 km s(-1) Mpc(-1). Finally, we compare these results with other, global methods for measuring H-o.