The H <sub>0</sub> trouble: confronting non-thermal dark matter and phantom cosmology with the CMB, BAO, and Type Ia supernovae data
S. Santos da Costa, Dêivid R. da Silva, Á. S. de Jesus, Nelson Pinto-Neto, Farinaldo S. Queiroz
Abstract
Abstract We have witnessed different values of the Hubble constant being found in the literature in the past years. Albeit, early measurements often result in an H 0 much smaller than those from late-time ones, producing a statistically significant discrepancy, and giving rise to the so-called Hubble tension. The trouble with the Hubble constant is often treated as a cosmological problem. However, the Hubble constant can be a laboratory to probe cosmology and particle physics models. In our work, we will investigate if the possibility of explaining the H 0 trouble using non-thermal dark matter production aided by phantom-like cosmology is consistent with the Cosmic Background Radiation (CMB) and Baryon Acoustic Oscillation (BAO) data. We performed a full Monte Carlo simulation using CMB and BAO datasets keeping the cosmological parameters Ω b h 2 , Ω c h 2 , 100θ, τ opt , and w as priors and concluded that a non-thermal dark matter production aided by phantom-like cosmology yields at most H 0 = 70.5 km s -1 Mpc -1 which is consistent with some late-time measurements. However, if H 0 > 72 km s -1 Mpc -1 as many late-time observations indicate, an alternative solution to the Hubble trouble is needed. Lastly, we limited the fraction of relativistic dark matter at the matter-radiation equality to be at most 1%.