Статья

Final Results from the<i>Hubble Space Telescope</i>Key Project to Measure the Hubble Constant

Wendy L. FreedmanThe Observatories, Carnegie Institution of Washington, Pasadena, CA 91101Barry F. MadoreNASA/IPAC Extragalactic Database, California Institute of Technology, Pasadena, CA 91125Brad K. GibsonCentre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, AustraliaLaura FerrareseRutgers University, New Brunswick, NJ 08854Daniel D. KelsonDepartment of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015Shoko SakaiNational Optical Astronomy Observatories, PO Box 26732, Tucson, AZ 85726Jeremy R. MouldResearch School of Astronomy and Astrophysics, Australian National University, Weston Creek Post Office, Weston, ACT, Australia 2611Robert C. Kennicutt, Jr.Steward Observatory, University of Arizona, Tucson, AZ 85721Holland C. FordDepartment of Physics and Astronomy, Bloomberg 501, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218John A. GrahamDepartment of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015John P. HuchraHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138Shaun M. G. HughesInstitute of Astronomy, Madingley Road, Cambridge CB3 0HA, UKGarth D. IllingworthLick Observatory, University of California, Santa Cruz, CA 95064Lucas M. MacriHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138Peter B. StetsonDominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council, 5071 West Saanich Road, Victoria, BC V8X 4M6, Canada

2001en

ABI

Аннотация

We present here the final results of the Hubble Space Telescope (HST) Key Project to measure the Hubble constant. We summarize our method, the results, and the uncertainties, tabulate our revised distances, and give the implications 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 recent improvements and refinements, including (1) a larger LMC Cepheid sample to define the fiducial period-luminosity (PL) relations, (2) a more recent HST Wide Field and Planetary Camera 2 (WFPC2) photometric calibration, (3) a correction for Cepheid metallicity, and (4) a correction for incompleteness bias in the observed Cepheid PL samples. We adopt a distance modulus to the LMC (relative to which the more distant galaxies are measured) of μ0 = 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 Cepheid data. The new calibration results in a Cepheid distance to NGC 4258 in better agreement with the maser distance to this galaxy. Based on these revised Cepheid distances, we find values (in km s-1 Mpc-1) of H0 = 71 ± 2 ± 6 (systematic) (Type Ia supernovae), H0 = 71 ± 3 ± 7 (Tully-Fisher relation), H0 = 70 ± 5 ± 6 (surface brightness fluctuations), H0 = 72 ± 9 ± 7 (Type II supernovae), and H0 = 82 ± 6 ± 9 (fundamental plane). We combine these results for the different methods with three different weighting schemes, and find good agreement and consistency with H0 = 72 ± 8 km s-1 Mpc-1. Finally, we compare these results with other, global methods for measuring H0.

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Идентификаторы

DOI: 10.1086/320638

Цитирования и источники

Цитирований: 5Использованных источников: 0

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