Cepheid Calibrations from the Hubble Space Telescope of the Luminosity of Two Recent Type Ia Supernovae and a Redetermination of the Hubble Constant

By A. Riess, Weidong Li, P. Stetson, A. Filippenko, S. Jha, R. Kirshner, P. Challis, P. Garnavich, Ryan Chornock. 2004

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We report observations of two nearby Type Ia supernovae (SNe Ia) for which observations of Cepheid variables in the host galaxies have been obtained with the Hubble Space Telescope: SN 1994ae in NGC 3370 and SN 1998aq in NGC 3982. For NCG 3370, we used the Advanced Camera for Surveys to observe 64 Cepheids that yield a distance of 29 Mpc, the farthest direct measurement of Cepheids. We have measured emission lines from H II regions in both host galaxies that provide metallicity-dependent corrections to their period-luminosity relations. These two SNe Ia double the sample of "ideal" luminosity calibrators: objects with well-observed and well-calibrated light curves of typical shape and with low reddening. By comparing them to all similarly well-measured SNe Ia in the Hubble flow, we find that H0 = 73 ± 4 (statistical) ± 5 (systematic) km s-1 Mpc-1. A detailed analysis demonstrates that most of the past disagreement over the value of H0 as determined from SNe Ia is abated by the replacement of past, problematic data by more accurate and precise, modern data.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/96f4eeb792861ec22682706e3f73456639f33d5b

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Citations in the corpus

Type Ia Supernovae Are Good Standard Candles in the Near Infrared: Evidence from PAIRITEL (2007, background): “SNe Ia have been the key tomeasuring the Hubble constant (Freedman et al. 2001; Jha et al. 1999; Riess et al. 2005) and demonstrating cosmic acceleration (Riess et al. 1998; Perlmutter et al. 1999).”
A REDETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE FROM A DIFFERENTIAL DISTANCE LADDER (2009, background): “Progress in the former was presented by Riess et al. (2005, 2009), more than doubling the sample of high-quality calibrators by providing reliable calibration for four modern SNe Ia.”
SPECTROSCOPIC OBSERVATIONS OF LYMAN BREAK GALAXIES AT REDSHIFTS ∼4, 5, AND 6 IN THE GOODS-SOUTH FIELD (2009, background): “0 by including additional observations taken during the continuation of the original GOODS survey for high-redshift Type Ia supernovae (Riess et al. 2004, 2005).”
New Hubble Space Telescope Discoveries of Type Ia Supernovae at z ≥ 1: Narrowing Constraints on the Early Behavior of Dark Energy (2006, methodology): “The present local mass density: M ¼ 0:28 0:04, a consensus value when combining large-scale structure (LSS) measurements from the 2dF and SDSS of Mh (Tegmark et al. 2004; Cole et al. 2005) and the value of H0 from HST Cepheids (Freedman et al. 2001; Riess et al. 2005).”
IMPROVED DARK ENERGY CONSTRAINTS FROM ∼100 NEW CfA SUPERNOVA TYPE Ia LIGHT CURVES (2009, methodology): “Riess et al. (2005) reported 1+w = −0.02+0.13−0.19.”
The Hubble Constant: A Summary of the Hubble Space Telescope Program for the Luminosity Calibration of Type Ia Supernovae by Means of Cepheids (2006, background): “Riess et al. (2005) have excluded six calibrators as being too old or too heavily absorbed, yet we find for these six SNe Ia H0 ¼ 61:0 2:0, which is the samewithin statistics as for their four calibrators.”
A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, methodology): “…for identifying Cepheids from time-series optical data (see Table 1 and Figure 2) has been described extensively (Saha et al. 1996; Stetson 1996; Riess et al. 2005; Macri et al. 2006); details of the procedures followed for this sample are presented by H16, utilize the DAO suite of software…”
A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (2011, methodology): “In Cycle 11, members of our team began using ACS to measure Cepheids at optical wavelengths in the hosts of more modern SNe Ia (SN 1994ae by Riess et al. 2005; SN 1995al and SN 2002fk by Riess et al. 2009b) and in a more ideal anchor galaxy (NGC 4258 by Macri 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): ““Ideal” or suitable SNe Ia for calibrating H0 (given limited HST time) were defined by Riess et al. (2005) to be (1) observed before maximum light, (2) through low interstellar extinction (AV< 0.5 mag), (3) with the same instruments and filters as the SNe Ia in the Hubble flow (at that time…”
Improved Distances to Type Ia Supernovae with Multicolor Light-Curve Shapes: MLCS2k2 (2006, methodology): “In addition, Riess et al. (2005) use MLCS2k2 distances to show that various estimates of H0 from SNe Ia can be reconciled through the use of modern Cepheid and SN data, deriving H0 ¼ 73 4 (statistical) 5 (systematic) km s 1 Mpc 1.”
SN 2003du: 480 days in the life of a normal type Ia supernova (2007, methodology): “Recently, Riess et al. (2005) calibrated the luminosities of SN 1998aq and SN 1994ae by observing Cepheids in their host galaxies with theHubble Space Telescope.”
Nearby Supernova Factory Observations of SN 2005gj: Another Type Ia Supernova in a Massive Circumstellar Envelope (2006, background): “They continue to play a major role in ongoing efforts to determine the cause of this acceleration (Knop et al. 2003; Tonry et al. 2003; Riess et al. 2004; Astier et al. 2006) and in refining the determination of the Hubble constant (Riess et al. 2005).”