Simulation-based Large Scale structure cosmology
The Good, the Bad and the Ugly
Carol Cuesta-Lazaro
\{ \Omega_\mathrm{M} , \sigma_8, ... \}
Forward Theory
Gravity
N-body
Initial Conditions
Simulations
Effective Field theories
Galaxies
Empirical
Hydro
Forward Survey
Mask, fibres...
Summarise
Initial Conditions
Observation
25 \, h^{-1}\mathrm{Mpc}
Empirical halo-galaxy connection
Identify host Dark matter haloes
p(N_g|M_h)
p(N_g|M_h, f_\mathrm{env})
Central galaxies : CoM largest sub-halo
Satellite galaxies : particles in halo
p(
)
|
\mathrm{Cosmology}
N-point functions
Counts-in-cell
Wavelets
Marked tpcfs
kNNs
Voids
Optimise information on cosmological parameters
Robust Surprises
Summarise
Density-split clustering
\xi^{qg}(s, \mu)
Quintile-galaxy crosscorrelations
Voids
Clusters
Quintile autocorrelations
\xi^{qq}(s, \mu)
Voids
Clusters
Fisher Information
Dark Matter halos Quijote Simulations
BOSS CMASS DR12
0.45 ≤ 𝑧 ≤ 0.6
The Good
The Bad
The Ugly
Simulations can model non-linear clustering
Forward modelling + ML = constraints from any summary
Ad-hoc galaxy-halo connection
Halos are social constructs
Limited number of simulations, prior limited
Difficult to estimate robust model errors
deck
By carol cuesta
