Conveners
Halo Theory: Boundary dynamics
- Surhud More (IUCAA)
Halo Theory: Boundary dynamics
- Surhud More (IUCAA)
I will report our recent development of the depletion radius, which is a new but fundamental halo boundary stemming from the macroscopic physics of halo growth. I will show that the depletion radius is both an important physical probe of halo evolution and a concise geometric boundary for halo models of the large scale structure, capable of overcoming major limitations of the classical halo in...
We determine the depletion radius from the stacked mass flow rate (MFR) profiles of dark matter haloes in a cosmological simulation and explore its dependence on halo properties. We find that the MFR profiles exhibit near self-similarity for haloes with different masses. The primary factor that determines the depletion radius is still the mass accretion rate, and the relation is similar to...
Splashback radius is a physically motivated boundary of halos, formed at the first apocenters of orbiting matter. Due to its strong correlation to the recent mass accretion history, especially that over the last one dynamical time, the splashback radius could be used to study the cosmic evolution, as well as astrophysics within halos. In this talk, I will briefly summarize the recent progress...
We investigate the splashback features of nonspherical dark-matter halos in phase space, namely based on cosmic density and velocity fields. Besides the density correlation function binned by the halo orientation angle, which was used in the literature, we introduce the corresponding velocity statistic, alignment velocity correlation function, to consider halo's asphericity. Using...
Clusters of galaxies are massive bound systems. At a large radius of 5 Mpc or more, massive clusters of galaxies decouple from the Hubble flow. Within this turnaround radius, galaxies are still accreting onto the cluster in the outer portion, the infall region. In the dense central regions with radii < 2 Mpc, clusters are dynamically relaxed. We use the radial velocity profile of cluster...
