Interpret the requested abundance as comoving number density and use this question's mean density, rather than importing the different cosmology of Question 2. The mass-to-radius relation for a spherical top-hat window function gives
The normalization radius is , not . Using ,
These are linearly extrapolated rms amplitudes, even when the numerical value at late times exceeds one. The high-redshift matter-dominated approximation is appropriate to the crossing sought below.
For , the Press-Schechter halo mass function yields
Equating this to gives . On the rare-object branch, solving gives . Hence
This is the first crossing as the Universe evolves from very early times. It retains the supplied scale-free extrapolation across a substantial range of scales; it is not a precision prediction using a full matter spectrum.
The abundance factor peaks at . Therefore the same target has a second mathematical root, , corresponding to if matter-dominated growth is extrapolated indefinitely. This extremely remote future branch is not the formation epoch and would not be physically justified by that growth approximation in a universe with late vacuum domination. This illustrates the two abundance crossings of the Press-Schechter mass function.
There is also an input-normalization qualification. If the characteristic cutoff is defined exactly by , the variance normalization here gives , rather than the earlier approximate quoted cutoff. The numerical estimate uses the explicit rms normalization in this part and the mass-scaling exponent from the preceding part; both cutoff normalizations cannot be imposed as exact simultaneously.