Conveners
Halo model of LSS
- James Taylor (Waterloo Centre for Astrophysics)
Halo model of LSS
- James Taylor (Waterloo Centre for Astrophysics)
The halo model is a powerful tool for understanding the non-linear evolution of the Universe. Conventionally, a dark matter halo is defined as a virialized object according to the virial radius. However, this definition does not completely partition all mass into halos, as the halo is much more extended beyond the virial radius and grows continuously. Consequently, there is a well-known...
The standard halo model of large-scale structure provides an empirically-informed framework for describing nonlinear structures in the universe. However, this model does not enforce conservation laws, which can significantly hinder observable predictions on large scales. Examples of these observables include weak lensing, as the power spectrum is overpredicted by $\geq 8\%$ on scales larger...
Secondary bias reflects the fact that large-scale clustering of haloes at a given mass varies significantly with their secondary properties. Recent studies identify tidal anisotropy, defined on intermediate scales, as the primary driver of secondary bias. Essentially, the tidal field is tightly intertwined with the large-scale matter distribution. In this work, we investigate the intricate...
I will introduce the dynamical halo model, a re-imagining of the traditional halo model built on the orbiting/infall dichotomy of particles around halos. We will introduce the basic ideas behind the dynamical halo model, some of the physical insights it provides that can improve our descriptions of large scale structure, and new tools we are developing to make the use of dynamical halos...
Building on a dynamics-based halo model proposed by Salazar [Edgar M. Salazar et al., arXiv:2406.04054], we compare the halo radius derived from the halo-mass correlation function with that from the halo-galaxy correlation function. The discrepancy between these two radii shows a strong dependence on halo mass and galaxy mass. To explain this relationship, we have developed a dynamical...
We present an analysis of the splashback radius ($R_{\text{sp}}$) and the associated splashback mass ($M_{\text{sp}}$) for a sample of galaxy clusters using SDSS spectroscopic data and mock simulations. $R_{\text{sp}}$ marks a physical boundary between the virialized core and the outer infall regions of clusters, providing a robust measure of cluster mass accretion history without being...
