A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations

Abstract

We present a new calibration of the peak absolute magnitude of Type Ia supernovae (SNe Ia) based on the surface brightness fluctuations (SBF) method, aimed at measuring the value of the Hubble constant. We build a sample of calibrating anchors consisting of 24 SNe hosted in galaxies that have SBF distance measurements. Applying a hierarchical Bayesian approach, we calibrate the SN Ia peak luminosity and extend the Hubble diagram into the Hubble flow by using a sample of 96 SNe Ia in the redshift range 0.02 < z < 0.075, which was extracted from the Combined Pantheon Sample. We estimate a value of H0 = 70.50 ± 2.37 (stat.) ± 3.38 (sys.) km s−1 Mpc−1 (i.e., 3.4% stat., 4.8% sys.), which is in agreement with the value obtained using the tip of the red giant branch calibration. It is also consistent, within errors, with the value obtained from SNe Ia calibrated with Cepheids or the value inferred from the analysis of the cosmic microwave background. We find that the SNe Ia distance moduli calibrated with SBF are on average larger by 0.07 mag than those calibrated with Cepheids. Our results point to possible differences among SNe in different types of galaxies, which could originate from different local environments and/or progenitor properties of SNe Ia. Sampling different host galaxy types, SBF offers a complementary approach to using Cepheids, which is important in addressing possible systematics. As the SBF method has the ability to reach larger distances than Cepheids, the impending entry of the Vera C. Rubin Observatory and JWST into operation will increase the number of SNe Ia hosted in galaxies where SBF distances can be measured, making SBF measurements attractive for improving the calibration of SNe Ia, as well as in the estimation of H0.

Can Hubble Tension Be Eased by Invoking a Finite Range for Gravity?

“…−1[16], midway between the values from Planck and SH0ES. The most recent calibration of Type Ia supernova based on the surface brightness fluctuations (SBF) method consisting of 24 supernovae hosted in galaxies that have SBF distance measurements estimated a value of 70.50 ± 3.38 −1 −1[17]. This is in good agreement with that obtained from the TRGB calibration.…”

Cosmological constraints from H ii starburst galaxy apparent magnitude and other cosmological measurements

“…Second, the HzBSNPDQH combination strongly disfavors nonflat ΛCDM, flat XCDM, and flat φCDM, and very strongly disfavors non-flat XCDM and non-flat φCDM. Furthermore, 10 Other local expansion rate H 0 measurements result in slightly lower central values with slightly larger error bars (Rigault et al 2015;Zhang et al 2017;Dhawan et al 2018;Fernández Arenas et al 2018;Breuval et al 2020;Efstathiou 2020;Khetan et al 2021;Rameez & Sarkar 2021;Freedman 2021). Our H 0 estimates are consistent with earlier median statistics determinations (Gott et al 2001;Calabrese et al 2012) as well as with other recent H 0 measurements (Chen et al 2017;DES Collaboration 2018;Gómez-Valent & Amendola 2018;Planck Collaboration 2020;Domínguez et al 2019;Cuceu et al 2019;Zeng & Yan 2019;Schöneberg et al 2019;Blum et al 2020;Lyu et al 2020;Philcox et al 2020;Birrer et al 2020;Denzel et al 2021;Pogosian et al 2020;Boruah et al 2021;Kim et al 2020…”

A buyer’s guide to the Hubble constant

“…Promising methods that we did not have space to discuss are Surface Brightness Fluctuations (Tonry and Schneider 1988;Blakeslee et al 2021;Khetan et al 2021), Cosmic Chronometers (Jimenez and Loeb 2002;Moresco et al 2018), the Tully-Fisher relation (Tully and Fisher 1977;Kourkchi et al 2020;Schombert et al 2020), Type II supernovae (de Jaeger et al 2020), HII galaxies (Terlevich and Davies 1981;Arenas et al 2018), andGalaxy Parallax (Croft 2021). Quasars (Risaliti and Lusso 2019) and GRBs (Schaefer 2007) offer the prospect of extending the Hubble diagram up to z $ 5, further testing KCDM.…”