The LCDM model has the virtue of having strong predictive power in so
far as the properties of the dark matter are concerned. For example,
the mass function of dark matter halos is known to high precision,
from the mass scale of the Earth to that of rich clusters. The
predictive power is weakened when baryons are considered because of
the complex astrophysical processes to which they can...
Every dark matter halo forms with a ρ ∝ r−1.5 density cusp at its center. This prompt cusp has a mass comparable to the cutoff scale in the spectrum of initial density perturbations. For warm and interacting dark matter models, prompt cusps significantly influence the structures of low-mass halos, so they are an important consideration for efforts to use satellite galaxies, strong...
I will present recent high-resolution N-body simulations of self-interacting dark matter (SIDM) and discuss their implications across a broad range of astrophysical observations. In particular, I will highlight novel signatures arising from gravothermal collapse in dark matter halos. I will then explore the prospects for detecting these signatures in strong gravitational lensing systems,...
The Nuclear Star Cluster (NSC) is at the centre of the Galaxy, an extremely dense star system. Several mechanisms are exists to explain how NSCs form, including gas migrating or GCs merging to the NSC.
Based on the second idea, we will present the processes involved in the complete decay of GCs during their interaction with the NSC of our Galaxy.
We have generated 'theoretical' GCs in a...
The LCDM model has ben challenged many times in the past decade,
mainly by galaxy observations on small scales: from the abundance of
satellites, to the distribution of dark matter within galaxies. In my talk
I will first revise all these claims with the help of cosmological
numerical simulations of galaxy formation from the NIHAO project. I will
then discuss whether there is indeed an...
