| Title: |
The Hubble Space Telescope key project on the extragalactic distance scale XXVIII: combining the constraints on the Hubble constant |
| Authors: |
Mould, Jeremy R.; Huchra, John P.; Freedman, Wendy L.; Kennicutt Jr, Robert C.; Ferrarese, Laura; Ford, Holland C.; Gibson, Brad K.; Graham, John A.; Hughes, Shaun M. G.; Illingworth, Garth D.; Kelson, Daniel D.; Macri, Lucas M.; Madore, Barry F.; Sakai, Shoko; Sebo, Kim M.; Silbermann, Nancy A.; Stetson, Peter B. |
| Contributors: |
Swinburne University of Technology |
| Source: |
Astrophysical Journal, Vol. 529, no. 2 (Feb 2000), pp. 786-794 |
| Publisher Information: |
University of Chicago Press |
| Publication Year: |
2000 |
| Collection: |
Swinburne University of Technology: Swinburne Research Bank |
| Description: |
Since the launch of Hubble Space Telescope (HST) 9 yr ago, Cepheid distances to 25 galaxies have been determined for the purpose of calibrating secondary distance indicators. Eighteen of these have been measured by the HST Key Project team, six by the Supernova Calibration Project, and one independently by Tanvir. Collectively, this work sets out an array of survey markers over the region within 25 Mpc of the Milky Way. A variety of secondary distance indicators can now be calibrated, and the accompanying four papers employ the full set of 25 galaxies to consider the Tully-Fisher relation, the fundamental plane of elliptical galaxies, Type Ia supernovae, and surface brightness fluctuations. When calibrated with Cepheid distances, each of these methods yields a measurement of the Hubble constant and a corresponding measurement uncertainty. We combine these measurements in this paper, together with a model of the velocity field, to yield the best available estimate of the value of H0 within the range of these secondary distance indicators and its uncertainty. The uncertainty in the result is modeled in an extensive simulation we call the 'virtual Key Project.' The velocity-field model includes the influence of the Virgo cluster, the Great Attractor, and the Shapley supercluster, but does not play a significant part in determining the result. The result is H0 = 71 ± 6 km s-1 Mpc-1. The largest contributor to the uncertainty of this 67% confidence level result is the distance of the Large Magellanic Cloud, which has been assumed to be 50 ± 3 kpc. This takes up the first 6.5% of our 9% error budget. Other contributors are the photometric calibration of the WFPC2 instrument, which takes up 4.5%, deviations from uniform Hubble flow in the volume sampled (lesssim2%), the composition sensitivity of the Cepheid period-luminosity relation (4%), and departures from a universal reddening law (~1%). These are the major components that , when combined in quadrature, make up the 9% total uncertainty. If the LMC distance modulus ... |
| Document Type: |
article in journal/newspaper |
| Language: |
unknown |
| Relation: |
http://hdl.handle.net/1959.3/210921; https://doi.org/10.1086/308304 |
| DOI: |
10.1086/308304 |
| Availability: |
http://hdl.handle.net/1959.3/210921; https://doi.org/10.1086/308304 |
| Rights: |
Copyright © 2000 The American Astronomical Society. |
| Accession Number: |
edsbas.20F1ACDC |
| Database: |
BASE |