Mass assembly history of dark matter halos in the light of $H_0$ tension

Abstract

The Hubble tension may introduce a new course of action to revise the standard ΛCDM model to unravel dark energy and dark matter physics. The Hubble parameter can be reconstructed by late-time observations of the background evolution model independently to reconciles the Hubble tension. We relate the reconstructed Hubble parameter to the structure formation and large scale structure observables in this work. We use the excursion set theory to calculate the number density of dark matter halos, the distribution of sub-halo progenitors, and dark matter halos' merger rate. We obtain the results for both the Markov and non-Markov extension of the excursion set theory. We show that the number density of dark matter halos in the reconstructed model has a ∼ 2σ difference in comparison to the Planck-2018 ΛCDM in the mass range of M < 10 12 M . We also compare the dark matter halo merger rate with the pair-galaxy statistics and their merger rate from observational data of HST, CANDEL survey. We assert a ∼ 5 times more accurate observations in the redshift range of z 0.75 − 2.5 can distinguish the reconstructed model and the Planck-2018 ΛCDM.

Primordial Black Holes in the Excursion Set Theory

“…We will produce Markov trajectories by the method developed in our previous works [35,36,37] where the distribution of DM halos in the (extended) standard model are addressed in more detail. It is worth to mention that there is an important and fundamental difference between the statistics of DM halos and PBHs.…”