| Authors | Sakai, Shoko; Mould, Jeremy R.; Hughes, Shaun M. G.; Huchra, John P.; Macri, Lucas M.; Kennicutt, Robert C., Jr.; Gibson, Brad K.; Ferrarese, Laura; Freedman, Wendy L.; Han, Mingsheng; Ford, Holland C.; Graham, John A.; Illingworth, Garth D.; Kelson, Daniel D.; Madore, Barry F.; Sebo, Kim; Silbermann, N. A.; Stetson, Peter B. |
| Abstract | This paper presents the calibration of BVRIH-0.5 Tully-Fisher relations based on Cepheid distances to 21 galaxies within 25 Mpc and 23 clusters within 10,000 km s-1. These relations have been applied to several distant cluster surveys in order to derive a value for the Hubble constant, H0, mainly concentrating on an I-band all-sky survey by Giovanelli and collaborators, consisting of total I magnitudes and 50% line width data for ~550 galaxies in 16 clusters. For comparison, we also derive the values of H0 using surveys in the B and V bands by Bothun and collaborators, and in H band by Aaronson and collaborators. Careful comparisons with various other databases from the literature suggest that the H-band data, which have isophotal magnitudes extrapolated from aperture magnitudes rather than total magnitudes, are subject to systematic uncertainties. Taking a weighted average of the estimates of Hubble constants from four surveys, we obtain H0=71+/-4 (random)+/-7 (systematic). We have also investigated how the value of H0 is affected by various systematic uncertainties, such as the internal extinction correction method used, Tully-Fisher slopes and shapes, a possible metallicity dependence of the Cepheid period-luminosity relation, and cluster population incompleteness bias. |
