Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant

<!DOCTYPE html>     <html class="no-js" lang="en">  <head> <title>Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant - NASA/ADS</title>  <link rel="apple-touch-icon" sizes="180x180" href="//styles/favicon/apple-touch-icon.png" /> <link rel="icon" type="image/png" sizes="32x32" href="//styles/favicon/favicon-32x32.png" /> <link rel="icon" type="image/png" sizes="16x16" href="//styles/favicon/favicon-16x16.png" /> <link rel="manifest" href="//styles/favicon/site.webmanifest" /> <link rel="mask-icon" href="//styles/favicon/safari-pinned-tab.svg" color="#5bbad5" /> <meta name="apple-mobile-web-app-title" content="NASA ADS" /> <meta name="application-name" content="NASA ADS" /> <meta name="msapplication-TileColor" content="#ffc40d" /> <meta name="theme-color" content="#ffffff" />  <link rel="stylesheet" href="/styles/css/styles.css"> <meta name="robots" content="noarchive"> <link rel="canonical" href="http://ui.adsabs.harvard.edu/abs/2001ApJ...553...47F/abstract"/> <meta name="description" content="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 渭<SUB>0</SUB>(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 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<SUP>-1</SUP> Mpc<SUP>-1</SUP>) of H<SUB>0</SUB>=71+/-2 (random)+/-6 (systematic) (Type Ia supernovae), H<SUB>0</SUB>=71+/-3+/-7 (Tully-Fisher relation), H<SUB>0</SUB>=70+/-5+/-6 (surface brightness fluctuations), H<SUB>0</SUB>=72+/-9+/-7 (Type II supernovae), and H<SUB>0</SUB>=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 H<SUB>0</SUB>=72+/-8 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>. Finally, we compare these results with other, global methods for measuring H<SUB>0</SUB>. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555.">  <meta property="og:type" content="article"> <meta property="og:title" content="Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant"> <meta property="og:site_name" content="NASA/ADS"> <meta property="og:description" content="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 渭<SUB>0</SUB>(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 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<SUP>-1</SUP> Mpc<SUP>-1</SUP>) of H<SUB>0</SUB>=71+/-2 (random)+/-6 (systematic) (Type Ia supernovae), H<SUB>0</SUB>=71+/-3+/-7 (Tully-Fisher relation), H<SUB>0</SUB>=70+/-5+/-6 (surface brightness fluctuations), H<SUB>0</SUB>=72+/-9+/-7 (Type II supernovae), and H<SUB>0</SUB>=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 H<SUB>0</SUB>=72+/-8 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>. Finally, we compare these results with other, global methods for measuring H<SUB>0</SUB>. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555."> <meta property="og:url" content="https://ui.adsabs.harvard.edu/abs/2001ApJ...553...47F/abstract"> <meta property="og:image" content="https://ui.adsabs.harvard.edu/styles/img/transparent_logo.svg"> <meta property="article:published_time" content="05/2001"> <meta property="article:author" content="Freedman, Wendy L."> <meta property="article:author" content="Madore, Barry F."> <meta property="article:author" content="Gibson, Brad K."> <meta property="article:author" content="Ferrarese, Laura"> <meta property="article:author" content="Kelson, Daniel D."> <meta property="article:author" content="Sakai, Shoko"> <meta property="article:author" content="Mould, Jeremy R."> <meta property="article:author" content="Kennicutt, Robert C., Jr."> <meta property="article:author" content="Ford, Holland C."> <meta property="article:author" content="Graham, John A."> <meta property="article:author" content="Huchra, John P."> <meta property="article:author" content="Hughes, Shaun M. 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G."> <meta name="dc.creator" content="Illingworth, Garth D."> <meta name="dc.creator" content="Macri, Lucas M."> <meta name="dc.creator" content="Stetson, Peter B.">  <meta name="twitter:card" content="summary_large_image"/> <meta name="twitter:description" content="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 渭<SUB>0</SUB>(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 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<SUP>-1</SUP> Mpc<SUP>-1</SUP>) of H<SUB>0</SUB>=71+/-2 (random)+/-6 (systematic) (Type Ia supernovae), H<SUB>0</SUB>=71+/-3+/-7 (Tully-Fisher relation), H<SUB>0</SUB>=70+/-5+/-6 (surface brightness fluctuations), H<SUB>0</SUB>=72+/-9+/-7 (Type II supernovae), and H<SUB>0</SUB>=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 H<SUB>0</SUB>=72+/-8 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>. Finally, we compare these results with other, global methods for measuring H<SUB>0</SUB>. 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<li class="author"><a href="/search/?q=author%3A%22Madore%2C+Barry+F.%22">Madore, Barry F.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Gibson%2C+Brad+K.%22">Gibson, Brad K.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Ferrarese%2C+Laura%22">Ferrarese, Laura</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Kelson%2C+Daniel+D.%22">Kelson, Daniel D.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Sakai%2C+Shoko%22">Sakai, Shoko</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Mould%2C+Jeremy+R.%22">Mould, Jeremy R.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Kennicutt%2C+Robert+C.%2C+Jr.%22">Kennicutt, Robert C., Jr.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Ford%2C+Holland+C.%22">Ford, Holland C.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Graham%2C+John+A.%22">Graham, John A.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Huchra%2C+John+P.%22">Huchra, John P.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Hughes%2C+Shaun+M.+G.%22">Hughes, Shaun M. G.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Illingworth%2C+Garth+D.%22">Illingworth, Garth D.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Macri%2C+Lucas+M.%22">Macri, Lucas M.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Stetson%2C+Peter+B.%22">Stetson, Peter B.</a> </li> </ul> </div> <div class="s-abstract-text"> <h4 class="sr-only">Abstract</h4> <p> 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 渭<SUB>0</SUB>(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 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<SUP>-1</SUP> Mpc<SUP>-1</SUP>) of H<SUB>0</SUB>=71+/-2 (random)+/-6 (systematic) (Type Ia supernovae), H<SUB>0</SUB>=71+/-3+/-7 (Tully-Fisher relation), H<SUB>0</SUB>=70+/-5+/-6 (surface brightness fluctuations), H<SUB>0</SUB>=72+/-9+/-7 (Type II supernovae), and H<SUB>0</SUB>=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 H<SUB>0</SUB>=72+/-8 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>. Finally, we compare these results with other, global methods for measuring H<SUB>0</SUB>. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. </p> </div> <br> <dl class="s-abstract-dl-horizontal"> <dt>Publication:</dt> <dd> <div id="article-publication">The Astrophysical Journal</div> </dd> <dt>Pub Date:</dt> <dd>May 2001</dd> <dt>DOI:</dt> <dd> <span> <a href="/link_gateway/2001ApJ...553...47F/doi:10.1086/320638" target="_blank" rel="noopener">10.1086/320638</a> <i class="fa fa-external-link"></i> </span> </dd> <dt>arXiv:</dt> <dd> <span> <a href="/link_gateway/2001ApJ...553...47F/arXiv:astro-ph/0012376" target="_blank" rel="noopener">arXiv:astro-ph/0012376</a> <i class="fa fa-external-link"></i> </span> </dd> <dt>Bibcode:</dt> <dd> <a href="/abs/2001ApJ...553...47F/abstract"> 2001ApJ...553...47F </a> <i class="icon-help" title="The bibcode is assigned by the ADS as a unique identifier for the paper."></i> </dd> <dt>Keywords:</dt> <dd> <ul class="list-inline"> <li>Stars: Variables: Cepheids;</li> <li>Cosmology: Observations;</li> <li>Cosmology: Distance Scale;</li> <li>Galaxies: Distances and Redshifts;</li> <li>Astrophysics</li> </ul> </dd> <dt>E-Print:</dt> <dd> Accepted to the Astrophysical Journal, 10 figures </dd> </dl> </article> </div> <div data-widget="ShowCitations"></div> <div data-widget="ShowReferences"></div> <div data-widget="ShowCoreads"></div> <div data-widget="ShowSimilar"></div> <div data-widget="ShowTableofcontents"></div> <div data-widget="ShowGraphics"></div> <div data-widget="ShowExportcitation" data-origin="abstract"></div> <div data-widget="ShowMetrics" data-allow-redirect="false"></div> <div data-widget="MetaTagsWidget"></div> </div> </div> </div> <div class="s-right-col-container col-xs-12 col-sm-12 col-md-3 col-lg-2 s-right-column" id="right-col-container" > <div data-widget="ShowResources"> <div data-reactroot="" class="s-right-col-widget-container" style="padding: 10px" > <div> <div 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Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant - NASA/ADS