Measuring inflaton couplings via dark radiation as $ΔN_{eff}$ in CMB

We study the production of a beyond the Standard Model (BSM) free-streaming relativistic particles which contribute to 𝑁${eff}$ and investigate how much the predictions for the inflationary analysis change. We consider inflaton decay as the source of this dark radiation (DR) and use the cosmic microwave background (CMB) data from Planck-2018 to constrain the scenarios and identify the parameter space involving couplings and masses of the inflaton that will be within the reach of next-generation CMB experiments like SPT-3G, CMB-S4, CMB-Bhārat, PICO, CMB-HD, etc. We find that if the BSM particle is produced only from the interaction with inflaton along with Standard Model (SM) relativistic particles, then its contribution to 𝑁${eff}$ is a monotonically increasing function of the branching fraction, 𝐵$𝑋$ of the inflaton to the BSM particle 𝑋; Planck bound on 𝑁${eff}$ rules out such 𝐵$𝑋$ ≳0.09. Considering two different analyses of Planck+bicep data together with other cosmological observations, 𝑁${eff}$ is treated as a free parameter, which relaxes the constraints on scalar spectral index (𝑛$_𝑠$) and tensor-to-scalar ratio (𝑟). The first analysis leads to predictions on the inflationary models like hilltop inflation being consistent with the data. Second analysis rules out the possibility that BSM particle 𝑋 producing from the inflaton decay in Coleman-Weinberg inflation or Starobinsky inflation scenarios. To this end, we assume that SM Higgs is produced along with the BSM particle. We explore the possibilities that 𝑋 can be either a scalar or a fermion or a gauge boson and consider possible interactions with inflaton and find out the permissible range on the allowed parameter space Planck and those which will be within the reaches of future CMB observations.