Abstract:

The most stringent local measurement of the Hubble constant from Cepheid-calibrated Type Ia supernovae (SNe~Ia) differs from the value inferred via the cosmic microwave background radiation ({\it Planck}+ΛCDM) by more than 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 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 dataset, 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 tension 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.