Global textures and the formation of self-bound gravitational systems

Using a Newtonian approximation we developed a quantitative criterion for the collapse of a spherical distribution of matter under an isolated texture field. In particular, we found the evolution of an overdense region is strongly determined by two parameters: the energy scale of symmetry breaking ( η ) and the initial radius of the system. Applying our collapse criterion to typical galaxy scales we verified the formation of 10¹¹‐M_⊙ objects at z ≲9 and 10¹²‐M_⊙ objects at z ≲5.