# Perturbations in Tachyon Dark Energy and their Effect on Matter Clustering

## TL;DR

This paper investigates how perturbations in tachyon dark energy influence matter clustering and compares these effects with the standard b1CDM model, providing new constraints and reducing data tension.

## Contribution

It introduces the study of tachyon field perturbations on matter clustering, considering two potentials, and demonstrates their role in alleviating data-model tensions.

## Key findings

- Dark energy perturbations are negligible at sub-Hubble scales but significant at super-Hubble scales.
- Growth rate of matter is suppressed in tachyon models during dark energy domination.
- Perturbations in tachyon fields help reduce tension between growth rate data and CMB observations.

## Abstract

A non-canonical scalar tachyon field is a viable candidate for dark energy and has been found to be in good agreement with observational data. Background data alone cannot completely rule out degeneracy between this model and others. To further constrain the parameters, apart from the distance measurements, we study perturbations in the tachyon scalar field and how they affect matter clustering. We consider two tachyon potentials for this study, an inverse square potential and an exponential potential. We study the evolution of the gravitational potential, matter density contrast, and dark energy density contrast, and compare them with the evolution in the $\Lambda CDM $ model. Although perturbations in dark energy at sub-Hubble scales are negligible in comparison with matter perturbations, they cannot be ignored at Hubble and super-Hubble scales ($\lambda_p > 1000$ Mpc). We also study the evolution of growth function and growth rate of matter, and find that the growth rate is significantly suppressed in dark energy dominated era with respect to the growth rate for $\Lambda CDM$ model. A comparison of these models with Redshift Space Distortion growth rate data is presented by way of calculating $f\sigma_8(z)$. There is a tension of $2.9\sigma$ ($2.26\sigma$ ) between growth rate data and Planck-2015 (Planck-2018) Cosmic Microwave Background Radiation data for $\Lambda CDM$ model. We present constraints on free parameters of these models and show that perturbations in the tachyon scalar field reduce this tension between different data sets.