Scalar Photon Coupling and Modified Photon Evolution: CMB Signatures and Cosmological Constraints

Abstract

We investigate the constant-$\epsilon$ limit of a photon-sector modification derived from an early-time interaction between a scalar field and radiation. Starting from the underlying scalar--photon coupling, the parameter $\epsilon$ quantifies the departure of the photon energy density from the standard adiabatic scaling, leading in the constant-$\epsilon$ limit to ${\rho }_{\gamma }\propto a^{-4+\epsilon }$ and to the modified CMB temperature--redshift relation $T(z)=T_0(1+z{)}^{1-\epsilon /4}$. The standard photon sector is recovered for $\epsilon =0$. We implement the corresponding constant-$\epsilon$ background evolution in CLASS and verify that the numerical photon-density evolution reproduces the analytic scaling. We then examine the resulting changes in the recombination history, visibility function and CMB temperature-anisotropy spectrum. These CMB spectra are used only as diagnostic outputs since the coupled scalar--photon perturbation equations are not implemented self-consistently in the numerical calculation and a full CMB likelihood analysis is beyond the scope of the present work. As a preliminary statistical application, we interface the modified CLASS implementation with MontePython and analyze the Pantheon+SH0ES supernova likelihood together with BAO measurements. Within the adopted constant-$\epsilon$ framework, prior choices, data combination and fixed early Universe parameter setup, we obtain $\epsilon =0.0230\pm 0.0065$. The posterior is therefore centered on a positive value within this restricted analysis. Because the BAO predictions depend on the model-dependent drag scale and several early-Universe quantities are held fixed, this result should be interpreted as a conditional and preliminary constraint rather than as a full CMB-level determination or evidence for a resolution of the Hubble tension.

20 pages, 4 figs