# Efficient cold outflows driven by cosmic rays in high redshift galaxies and their global effects on the IGM

## TL;DR

This paper models galactic outflows driven by cosmic rays in high redshift galaxies, showing they can sustain large-scale winds even in low-mass galaxies and significantly influence the intergalactic medium's properties and thermal history.

## Contribution

It introduces semi-analytical models incorporating cosmic ray pressure, revealing their role in driving outflows and affecting the IGM, extending previous thermal-only models.

## Key findings

- Cosmic rays enable outflows in low-mass galaxies where thermal pressure fails.
- Cosmic ray driven winds reach larger distances in massive galaxies.
- IGM magnetic fields and cosmic rays impact the thermal history and gamma-ray observations.

## Abstract

We present semi-analytical models of galactic outflows in high redshift galaxies driven by both hot thermal gas and non-thermal cosmic rays. Thermal pressure alone may not sustain a large scale outflow in low mass galaxies (i.e $M\sim 10^8$~M$_\odot$), in the presence of supernovae (SNe) feedback with large mass loading. We show that inclusion of cosmic ray pressure allows outflow solutions even in these galaxies. In massive galaxies for the same energy efficiency, cosmic ray driven winds can propagate to larger distances compared to pure thermally driven winds. On an average gas in the cosmic ray driven winds has a lower temperature which could aid detecting it through absorption lines in the spectra of background sources. Using our constrained semi-analytical models of galaxy formation (that explains the observed UV luminosity functions of galaxies) we study the influence of cosmic ray driven winds on the properties of the intergalactic medium (IGM) at different redshifts. In particular, we study the volume filling factor, average metallicity, cosmic ray and magnetic field energy densities for models invoking atomic cooled and molecular cooled halos. We show that the cosmic rays in the IGM could have enough energy that can be transferred to the thermal gas in presence of magnetic fields to influence the thermal history of the intergalactic medium. The significant volume filling and resulting strength of IGM magnetic fields can also account for recent $\gamma$-ray observations of blazars.