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Putting flat ΛCDM in the (Redshift) bin
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DOI：10.1016/j.dark.2024.101464.png)
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Abstract
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Flat Lambda CDM cosmology is specified by two constant fitting parameters at the background level in the late Universe, the Hubble constant H-0 and matter density (today) Omega(m). Mathematically, H-0 and Omega(m) are either integration constants arising from solving ordinary differential equations or are directly related to integration constants. Seen in this context, if fits of the Lambda CDM model to cosmological probes at different redshifts lead to different (H-0, Omega(m)) parameters, this is a mismatch between mathematics and observation. Here, in mock observational Hubble data (OHD) (geometric probes of expansion history) we demonstrate evolution in distributions of best fit parameters with effective redshift. As a result, considerably different H-0, Omega(m)) best fits from Planck-Lambda CDM cannot be precluded in high redshift bins. We explore if OHD, Type Ia supernovae and standardisable quasar samples exhibit redshift evolution of best fit Lambda CDM parameters. In all samples, we confirm a decreasing H-0 and increasing Omega(m) trend with increasing bin redshift. Through comparison with mocks, we confirm that similar behaviour can arise randomly within the flat Lambda CDM model with probabilities as low as p = 0.0021 (3.1 sigma). We present complementary profile distribution analysis confirming the shifts in cosmological parameters in high redshift bins. In particular, we identify a redshift range where Planck (H-0, Omega(m)) values are disfavoured at 99.6% (2.9 sigma) confidence level in a combination of OHD and supernovae data.
Keywords:
Dark Energy
Lambda-CDM cosmology
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