The Hubble Constant: A Summary of the Hubble Space Telescope Program for the Luminosity Calibration of Type Ia Supernovae by Means of Cepheids

By A. Sandage, G. Tammann, A. Saha, Bernd Reindl, F. Macchetto, N. Washington, A. Basel, Noao, Stsci. 2006

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This is the final summary paper of our 15 yr program using the Hubble Space Telescope (HST) to determine the Hubble constant from the Cepheid-calibrated luminosity of Type Ia supernovae. Several recent developments have made it necessary to put the summary on H0 on a broader basis than we originally thought (see the four papers cited in the text). The new Cepheid distances of the subset of 10 galaxies, which were hosts of normal SNe Ia, give weighted mean luminosities in B, V, and I at maximum light of -19.49, -19.46, and -19.22, respectively. These calibrate the adopted SNe Ia Hubble diagram from Paper III to give H0 = 62.3 ± 1.3(random) ± 5.0(systematic) in units of km s-1 Mpc-1. This is a global value because it uses the Hubble diagram between redshift limits of 3000 and 20,000 km s-1, beyond the effects of any local random and streaming motions. Local values of H0 between 4.4 and 30 Mpc from Cepheids, SNe Ia, 21 cm line widths, and the tip of the red giant branch (TRGB) all agree within 5% of our global value. This agreement of H0 on all scales from ~4 to 200 Mpc finds its most obvious explanation in the smoothing effect of vacuum energy on the otherwise lumpy gravitational field due to the nonuniform distribution of the local galaxies. The present value of H0 is consistent with physical methods relying on the time delay of gravitational lenses and the Sunyaev-Zeldovich effect, and it is not in contradiction with the CMB data. Our value of H0 is 14% smaller than the value of H0 found by Freedman et al. because our independent Cepheid distances to the six SNe Ia-calibrating galaxies used in that analysis average 0.35 mag larger than those used earlier.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Hubble Space Telescope Fine Guidance Sensor Parallaxes of Galactic Cepheid Variable Stars: Period-Luminosity Relations (2006, background): “Two major groups have recently been or currently are involved in this effort, and their results are summarized in Freedman et al. (2001) and Sandage et al. (2006).”
Cosmological Constraints from a Combination of Galaxy Clustering and Lensing -- III. Application to SDSS Data (2012, background): “…stars by van Leeuwen et al. (2007) raises the value for h from the HST Key Project from 0.72±0.08km s−1 Mpc−1 (Freedman et al. 2001) to 0.76 ± 0.08 kms−1 Mpc−1 (68% CL), and the Cepheid-based determination of Sandage et al. (2006) from 0.62± 0.05 km s−1 Mpc−1 to 0.70± 0.05 kms−1 Mpc−1 (68% CL).”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, result): “Recent advances in the determination of the Hubble constant have been made since the two teams using HST/WFPC2 observations reported their results (Freedman et al. 2001; Sandage et al. 2006).”
A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team (2021, methodology): “This project was a “second-generation” effort to measure H0 with HST from a distance ladder of Cepheids and SNe Ia using the then recently installed ACS (and later WFC3) instruments, following successful efforts during the 1990s by the “first-generation” HST Key Project on the Extragalactic Distance”
A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (2011, methodology): “In the early Cycles of HST, the SN Ia HST Calibration Program (Sandage et al. 2006, hereafter SST) and the HST Key Project (Freedman et al. 2001, hereafter KP) each calibrated H0 via Cepheids and SNe Ia using the Wide Field Planetary Camera 2 (WFPC2) and the Large Magellanic Cloud (LMC) as the…”
The cluster gas mass fraction as a cosmological probe: a revised study (2009, background): “5.4) H0 = 62 0.37+0.04−0.04 0.63 +0.46 −0.48 0.35 +0.04 −0.05 1.15 +0.65 −0.40 H0 from Sandage et al. (2006) WMAP5 0.32+0.03−0.02 1.01 +0.20 −0.28 0.33 +0.02 −0.02 1.25 +0.35 −0.25 H0 and Ωb from Komatsu et al. (2008) The quoted constraints are obtained for each parameter after marginalization.”
H0LiCOW – XIII. A 2.4 per cent measurement of H0 from lensed quasars: 5.3σ tension between early- and late-Universe probes (2019, methodology): “Type Ia SNe luminosities are typically calibrated via the ‘distance ladder’ (e.g. Sandage et al. 2006; Freedman et al. 2012; Riess et al. 2016, 2018, 2019), in which parallax measurements are used to determine distances to nearby Cepheid variable stars (which have a known period–luminosity…”
A REDETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE FROM A DIFFERENTIAL DISTANCE LADDER (2009, methodology): “These Galactic Cepheids also have metallicities which are very similar to that of Cepheids in the SN hosts as discussed by Sandage et al. (2006).”
A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, methodology): “The SNIa HST Calibration Program (Sandage et al. 2006) and the HST Key Project (Freedman et al. 2001) both made use of HST observations with WFPC2 to resolve Cepheids in SNIa hosts.”