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