Combining pre- and post-recombination new physics to address cosmological tensions: case study with varying electron mass and sign-switching cosmological constant

Abstract

It has recently been argued that the Hubble tension may call for a combination of both pre- and post-recombination new physics. Motivated by these considerations, we provide one of the first concrete case studies aimed at constructing such a viable combination. We consider models that have individually worked best on either end of recombination so far: a spatially uniform time-varying electron mass leading to earlier recombination (also adding non-zero spatial curvature), and a sign-switching cosmological constant inducing an AdS-to-dS transition within the ${\Lambda }_{\mathrm{s}}$CDM model. When confronted against Cosmic Microwave Background (CMB), Baryon Acoustic Oscillations, and Type Ia Supernovae data, we show that no combination of these ingredients can successfully solve the Hubble tension. We find that the matter density parameter ${\Omega }_m$ plays a critical role, driving important physical scales in opposite directions: the AdS-to-dS transition requires a larger ${\Omega }_m$ to maintain the CMB acoustic scale fixed, whereas the varying electron mass requires a smaller ${\Omega }_m$ to maintain the redshift of matter-radiation equality fixed. Despite the overall failure, we use our results to draw general model-building lessons, highlighting the importance of assessing tension-solving directions in the parameter space of new physics parameters and how these correlate with shifts in other standard parameters, while underscoring the crucial role of ${\Omega }_m$ in this sense.

22 pages, 7 figures, 4 tables. Fig. 7 is the summary Figure. The reason for the failure of this particular combination of models and the consequent general lessons we draw are discussed between Pages 10 and 14. v2: several additional references added, minor change to title, added Bayesian evidence computation. Version accepted for publication in Phys. Dark Univ

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