TheHubble Space TelescopeKey Project on the Extragalactic Distance Scale. XXIV. The Calibration of Tully‐Fisher Relations and the Value of the Hubble Constant

Abstract

This paper presents the calibration ofTully-Fisher relations based on Cepheid distances BV RIH~0 .5 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, mainly concentrat-H 0 , ing on an I-band all-sky survey by Giovanelli and collaborators, consisting of total I magnitudes and 50% line width data for D550 galaxies in 16 clusters. For comparison, we also derive the values of H 0 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 (random)^7 (systematic). We have also H 0 \ 71^4 investigated how the value of is a †ected by various systematic uncertainties, such as the internal H 0 extinction correction method used, Tully-Fisher slopes and shapes, a possible metallicity dependence of the Cepheid period-luminosity relation, and cluster population incompleteness bias.

GMRTHI observations of the Eridanus group of galaxies

“…1. All these systems are Federspiel et al(1998), (2) Ferguson (1989), (3) Binggeli et al (1987), (4) Mushotzky & Smith (1980), (5) Mould et al (2000), (6) Richter & Sadler (1985), (7) Paolillo et al (2001), (8) Omar (2004), (9) Sakai et al (2000), (10) Tully et al (1996) at comparable distances. Both the Fornax cluster and the Eridanus group belong to the filamentary structure described by da Costa et al (1988).…”

From distances to galaxy evolution and the dark matter problem

“…Tully and Fisher succeeded in obtaining good calibrators with careful corrections, and then applied the relation to finding the distance to the Virgo and Ursa Major cluster. They also derived an estimate of the Hubble constant, H 0 = 80 km s −1 Mpc −1 , not so far from the accepted value today (Sakai et al 2000).The distance to Virgo that they determined (13.2 Mpc) was inconsistent with previous determinations of 19.5 Mpc (Sandage & Tammann 1974), and they argued that the reason was the previous inclusion of the Virgo II southern extension, which does not belong to the same cluster. An interesting feature of their work is that they proposed both the correlation of the HI line width with the magnitude and the diameter of spiral galaxies.…”

“…Tully and Fisher succeeded in obtaining good calibrators with careful corrections, and then applied the relation to finding the distance to the Virgo and Ursa Major cluster. They also derived an estimate of the Hubble constant, H 0 = 80 km s −1 Mpc −1 , not so far from the accepted value today (Sakai et al 2000).…”

Measuring the Hubble Constant With the Hubble Space Telescope

“…The first was the TullyFisher relation (Figure 18). Sakai et al (2000) obtained H 0 = 71 ± 3 ± 7 km s −1 Mpc −1 , where the first uncertainty is the random error and the second uncertainty is the systematic error.…”