# Constraining Dark Matter -- Dark Radiation interactions with CMB, BAO, and Lyman-$\alpha$

## TL;DR

This paper updates constraints on dark matter and dark radiation interactions using recent cosmological data, showing some models can alleviate the Hubble tension and small-scale structure issues.

## Contribution

It introduces a new Lyman-alpha likelihood and provides updated bounds on ETHOS models with different temperature scalings of DM-DR interactions.

## Key findings

- Lyman-alpha data significantly strengthen constraints for n=2 and 4 scenarios.
- Models with dark matter-dark radiation interactions can still address small-scale structure problems.
- Certain models reduce the Hubble tension from 4.1σ to 2.7σ.

## Abstract

Several interesting Dark Matter (DM) models invoke a dark sector leading to two types of relic particles, possibly interacting with each other: non-relativistic DM, and relativistic Dark Radiation (DR). These models have interesting consequences for cosmological observables, and could in principle solve problems like the small-scale cold DM crisis, Hubble tension, and/or low $\sigma_8$ value. Their cosmological behaviour is captured by the ETHOS parametrisation, which includes a DR-DM scattering rate scaling like a power-law of the temperature, $T^n$. Scenarios with $n=0$, $2$, or $4$ can easily be realised in concrete dark sector set-ups. Here we update constraints on these three scenarios using recent CMB, BAO, and high-resolution Lyman-$\alpha$ data. We introduce a new Lyman-$\alpha$ likelihood that is applicable to a wide range of cosmological models with a suppression of the matter power spectrum on small scales. For $n=2$ and $4$, we find that Lyman-$\alpha$ data strengthen the CMB+BAO bounds on the DM-DR interaction rate by many orders of magnitude. However, models offering a possible solution to the missing satellite problem are still compatible with our new bounds. For $n=0$, high-resolution Lyman-$\alpha$ data bring no stronger constraints on the interaction rate than CMB+BAO data, except for extremely small values of the DR density. Using CMB+BAO data and a theory-motivated prior on the minimal density of DR, we find that the $n=0$ model can reduce the Hubble tension from $4.1\sigma$ to $2.7\sigma$, while simultaneously accommodating smaller values of the $\sigma_8$ and $S_8$ parameters hinted by cosmic shear data.