Virial clouds evolution from the last scattering upto the formation of first stars

TL;DR

This paper explores the evolution of virial clouds from the last scattering surface to the formation of the first stars, aiming to understand their chemical composition and stability in the early universe.

Contribution

It provides a focused analysis of virial cloud evolution from the last scattering surface to early star formation, building on previous models of molecular hydrogen clouds in galactic halos.

Findings

Virial clouds could remain stable from the last scattering surface to star formation.

Chemical composition of these clouds influences their evolution and stability.

Model confrontation with observational data helps validate cloud stability hypotheses.

Abstract

The asymmetry in the cosmic microwave background (CMB) towards several nearby galaxies detected by Planck data is probably due to the rotation of "cold gas" clouds present in the galactic halos. In 1995 it had been proposed that galactic halos are populated by pure molecular hydrogen clouds which are in equillibrium with the CMB. More recently, it was shown that the equillibrium could be stable. Nevertheless, the cloud chemical composition is still a matter to be studied. To investigate this issue we need to trace the evolution of these virial cloud from the time of their formation to the present, and to confront the model with the observational data. The present paper is a short summary of a paper [1]. Here we only concentrate on the evolution of these clouds from the last scattering surface (LSS) up to the formation of first generation of stars (population-III stars).