2024ApJ...977..180R

Here we present an approach to the measurement of extragalactic distances using twin SNe Ia, taken from the early down to the nebular phase. The approach is purely empirical, although we can give a theoretical background on why the method is reliable. By studying those twins in galaxies where peculiar velocities are relatively unimportant, we can tackle the H₀ tension problem. Here we apply the method to the determination of the distances to NGC 7250 and NGC 2525, who hosted, respectively, SN 2013dy and SN 2018gv, twins of two different SNe Ia prototypes: SN 2013aa/SN 2017cbv and SN 2011fe. From the study of the SN 2013aa and SN 2017cbv twin pair, by comparing it with SN 2011fe and applying the difference between the SN 2013aa/2017cbv and the SN 2011fe class, we also find a good estimate of the distance to NGC 5643. We have just started to measure distances with the method for the samples in W.L Freedman et al. and A. G. Riess et al. There are differences in measured distances to the same galaxy using Cepheids or TRGBs. In this context of discrepancy, the “twins for life” method is very competitive because it can provide distance estimates with a modulus error of σ_μ = 0.04 mag. Our findings called for a revision of the distances measured with Cepheids in A. G. Riess et al. (2022). NGC 7250 and NGC 2525 needed better measurements with Cepheids. We have noticed that the Cepheids-based distance obtained with the JWST in A. G. Riess et al. (2024a) for NGC 5643 is in good agreement with what we find, unlike their previous estimate in A. G. Riess et al. (2022). The Hubble tension can arise from the way in which the local SNe Ia sample is linked to the SNe Ia Hubble flow sample. A good calibration of SNe Ia in the local sample is needed and we have started to gather it. We also expect to apply the “twin” SNe Ia comparison from the local sample to that in galaxies with z >0.02-0.03 well into the Hubble flow to obtain a reliable value for H₀. Those distant SNe Ia can be observed with the ELT or the JWST.