Impact of DESI BAO Data on Inflationary Parameters: stability against late-time new physics

TL;DR

This study assesses how DESI BAO data influences inflationary and cosmological parameters, finding stability in inflationary parameters across models and slight shifts in matter density and expansion rate when combined with other datasets.

Contribution

It demonstrates the stability of inflationary parameters with DESI BAO data across various late-time physics models and highlights subtle parameter shifts.

Findings

Inflationary parameters remain stable across models.

DESI BAO data slightly reduces matter density parameter.

Combined data leads to modest increases in $n_s$ and $H_0$.

Abstract

In this work, I investigate the impact of Dark Energy Spectroscopic Instrument (DESI) Baryonic Acoustic Oscillations (BAO) data on cosmological parameters, focusing on the inflationary spectral index $n_s$, the amplitude of scalar perturbations $A_s$, and the matter density parameter $\omega_m$. By examining different models of late-time new physics, the inflationary parameters were revealed to be stable when compared with the baseline dataset that used the earlier BAO data from the SDSS collaboration. When combined with Cosmic Microwave Background (CMB) and type Ia supernovae (SNeIa), DESI BAO data leads to a slight reduction in $\omega_m$ (less than 2\%) and modest changes in $A_s$ and $n_s$, if compared with the same combination but using SDSS BAO data instead, suggesting a subtle shift in matter clustering. These effects may be attributed to a higher expansion rate from dynamical dark energy, changes in the recombination period, or modifications to the matter-radiation equality time. Further analyses of models with dynamical dark energy and free curvature show a consistent trend of reduced $\omega_m$, accompanied by slight increases in both $n_s$ and $H_0$. The results emphasize the importance of the DESI BAO data in refining cosmological parameter estimates and highlight the stability of inflationary parameters across different late-time cosmological models.