Evolution of virial clouds-I: from surface of last scattering up to the formation of population-III stars

TL;DR

This paper investigates the early evolution of virial clouds from their formation before the first stars, aiming to understand their stability and role in cosmic microwave background interactions, based on observational data.

Contribution

It models the formation epoch of virial clouds and explores their potential equilibrium with the CMB, providing a foundation for future evolution studies.

Findings

Virial clouds could be in stable equilibrium with the CMB.

Temperature asymmetries in galaxy halos may be due to these clouds.

The formation process of such clouds before first star formation is analyzed.

Abstract

The analysis of WMAP and Planck CMB data has shown the presence of temperature asymmetries towards the halos of several galaxies, which is probably due to the rotation of clouds present in these halos about the rotational axis of the galaxies. It had been proposed that these are hydrogen clouds that {\it should} be in equilibrium with the CMB. However, standard theory did not allow equilibrium of such clouds at the very low CMB temperature, but it was recently shown that the equilibrium {\it could} be stable. This still does not prove that the cloud concentration and that the observed temperature asymmetry is due to clouds in equilibrium with the CMB. To investigate the matter further, it would be necessary to trace the evolution of such clouds, which we call "virial clouds", from their formation epoch to the present, so as to confront the model with the observational data. The task is to be done in two steps: (1) from the cloud formation before the formation of first generation of stars; (2) from that time to the present. In this paper we deal with the first step leaving the second one to a subsequent analysis.