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

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.

References in corpus (6)

• Formation of Massive Galaxies at High Redshift: Cold Streams, Clumpy Disks and Compact Spheroids
• Recovery from population III supernova explosions and the onset of second generation star formation
• Planck's confirmation of the M31 disk and halo rotation
• Triangulum galaxy viewed by Planck
• Virial clouds explaining the observed rotational asymmetry in the galactic halos
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Cited by in corpus (3)

• The rotational kinetic Sunyaev-Zeldovich contribution to the temperature asymmetry toward the M31 halo
• On the Galactic Halos Rotation by Planck Data
• The Baryonic Mass Estimates of the Milky Way Halo in the form of High Velocity Clouds