On redshift evolution and negative dark energy density in Pantheon plus Supernovae

Within the Friedmann-Lema & icirc;tre-Robertson-Walker (FLRW) framework, the Hubble constant H(0 )is an integration constant. Thus, consistency of the model demands observational constancy of H-0. We demonstrate redshift evolution of best fit Lambda CDM parameters(H-0,Omega(m))in Pantheon+supernove (SNe). Redshift evolution of best fit cosmological parameters is a prerequisite to finding a statistically significant evolution as well as identifying alternative models that are competitive with Lambda CDM in a Bayesian model comparison. To assess statistical significance, we employ three different methods: (i) Bayesian model comparison, (ii) mock simulations and (iii) profile distributions. The first shows a marginal preference for the vanilla Lambda CDM model over an adhoc model with 3 additional parameters and an unphysical jump in cosmological parameters at z=1. From mock simulations, we estimate the statistical significance of redshift evolution of best fit parameters and negative dark energy density (Omega(m)>1) to be in the 1-2 sigma range, depending on the criteria employed. Importantly, in direct comparison to the same analysis with the earlier Pantheon sample we find that statistical significance of redshift evolution of best fit parameters has increased, as expected for a physical effect. Our pro-file distribution analysis demonstrates a shift in(H-0,Omega(m))in excess of 95% confidence level for S Ne with redshifts z >1and also shows that a degeneracy in MCMC posteriors is not equivalent to a curve of constant chi (2). Our findings can be interpreted as a statistical fluctuation or unexplored systematics in Pantheon+ or Lambda CDM model breakdown. The first two possibilities are disfavoured by similar trends in independent probes