2022MNRAS.514.4620D

The most stringent local measurement of the Hubble-Lemaitre constant from Cepheid-calibrated Type Ia supernovae (SNe Ia) differs from the value inferred via the cosmic microwave background radiation (Planck+ΛCDM) by ∼5σ. This so-called Hubble tension has been confirmed by other independent methods, and thus does not appear to be a possible consequence of systematic errors. Here, we continue upon our prior work of using Type II supernovae to provide another, largely independent method to measure the Hubble-Lemaitre constant. From 13 SNe II with geometric, Cepheid, or tip of the red giant branch (TRGB) host-galaxy distance measurements, we derive H₀ = 75.4^+3.8_–3.7 km s^–1 Mpc^–1 (statistical errors only), consistent with the local measurement but in disagreement by ∼2.0σ with the Planck+ΛCDM value. Using only Cepheids (N = 7), we find H₀ = 77.6^+5.2_–4.8 km s^–1 Mpc^–1, while using only TRGB (N = 5), we derive H₀ = 73.1^+5.7_–5.3 km s^–1 Mpc^–1. Via 13 variants of our data set, we derive a systematic uncertainty estimate of 1.5 km s^–1 Mpc^–1. The median value derived from these variants differs by just 0.3 km s^–1 Mpc^–1 from that produced by our fiducial model. Because we only replace SNe Ia with SNe II - and we do not find statistically significant difference between the Cepheid and TRGB H₀ measurements - our work reveals no indication that SNe Ia or Cepheids could be the sources of the 'H₀ tension.' We caution, however, that our conclusions rest upon a modest calibrator sample; as this sample grows in the future, our results should be verified.