Carol Cuesta-Lazaro (IAIFI Fellow)

in collaboration with Siddarth Mishra-Sharma

Generative models for the Large Scale Structure

 

Why Carol loves generative models and thinks you should love them too

Initial Conditions of the Universe

Laws of gravity

3-D distribution of galaxies

Which are the ICs of OUR Universe?

Primordial non-Gaussianity?

Probe Inflation

Galaxy formation

3-D distribution of dark matter

Is GR modified on large scales?

How do galaxies form?

Neutrino mass hierarchy?

ML for Large Scale Structure:

A wish list

Generative models

Learn p(x)

Evaluate the likelihood of a 3D map, as a function of the parameters of interest

1

Combine different galaxy properties (such as velocities and positions)

2

Sample 3D maps from the posterior distribution 

3

p(
)
|
\mathrm{Cosmology}

"What I cannot create, I do not understand"

p(y|x)
p(x|y) = \frac{p(y|x)p(x)}{p(y)}
p(x|y)

https://vitalflux.com/generative-vs-discriminative-models-examples/

Hall of fame

A teddy bear wearing a motorcycle helmet and cape is standing in front of Loch Awe with Kilchurn Castle behind him driving a speed boat near the Golden Gate Bridge

 

https://parti.research.google​​​​​​​

Emulators of complex processes

Anomaly detection

arXiv:2010.11202

Estimating non-gaussian likelihoods

Model posterior distributions (uncertainties)

\mathcal{L}(y|\theta)

arXiv:2304.03788

Explicit Density

Implicit Density

Tractable Density

Approximate Density

Normalising flows

Variational Autoencoders 

Diffusion models

Generative Adversarial Networks

The zoo of generative models

z_T
z_{0}
z_{1}
z_{2}
p(z_{t-1}|z_t)
p(z_t|z_{t-1})

Reverse diffusion: Denoise previous step

Forward diffusion: Add Gaussian noise (fixed)

Diffusion models

A person half Yoda half Gandalf

z_T
z_{0}
z_{1}

Diffusion on 3D coordinates

z_{2}
q_\theta(z_{t-1}|z_t)
p(z_t|z_{t-1})

Reverse diffusion: Denoise previous step

Forward diffusion: Add Gaussian noise (fixed)

Cosmology

p(x,y,z|\Omega_m, \sigma_8)
p(x,y,z, v_x, v_y, v_z, M_h|\Omega_m, \sigma_8)

Density PDF

kNN

TPCF

Halo Mass Function

Velocity 

PDF

Mean pairwise velocity

z_T
z_{0}
z_{1}

Evidence Lower Bound (ELBO)

z_{2}
q_\theta(z_{t-1}|z_t) \approx p(z_{t-1}|z_{t})
p(z_t|z_{t-1})
p(z_{t-1}|z_{t})

Variational Inference

 Approximate the true posterior of the latent variables by a parametric distribution

\log p(\boldsymbol{x}) =
\geq \mathbb{E}_{q_{\boldsymbol{\phi}}(\boldsymbol{z}\mid\boldsymbol{x})}\left[\log\frac{p(\boldsymbol{x}, \boldsymbol{z})}{q_{\boldsymbol{\phi}}(\boldsymbol{z}\mid\boldsymbol{x})}\right]
\mathbb{E}_{q_{\boldsymbol{\phi}}(\boldsymbol{z}\mid\boldsymbol{x})}\left[\log\frac{p(\boldsymbol{x}, \boldsymbol{z})}{q_{\boldsymbol{\phi}}(\boldsymbol{z}\mid\boldsymbol{x})}\right] + \mathcal{D}_{\text{KL}}(q_{\boldsymbol{\phi}}(\boldsymbol{z}\mid\boldsymbol{x}) \mid\mid p(\boldsymbol{z}\mid\boldsymbol{x}))

Evidence Lower Bound

Distance to true posterior

q_\theta(z|x) \approx p(z|x)

  Find

1. ELBO is a lower bound of the evidence

2. Maximising ELBO = Minimising KL

Maximise ELBO to maximise ev/likelihood

Maximise ELBO to approximate true posterior

Setting tight constraints with only 5000 halo positions

 

+ Galaxy formation

+ Observational systematics (Cut-sky, Fiber collisions)

+ Lightcone, Redshift Space Distortions....

Forward Model

N-body simulations

Observations

 SIMBIG arXiv:2211.00723

We can simulate the observable Universe, we just need hydrodynamical simulations

25 \, h^{-1}\mathrm{Mpc}

What are subresolution models?

10^{10} - 10^{11} M_\odot

Super massive black hole seeding in dark matter halos

BH feedback impacts galactic scales

Black holes can also grow through mergers

Effective models of astrophysical processes needed due to limited numerical resolutions or limited physical models

they can even teleport!

F_\theta(\mathbf{x},a) = \frac{3 \Omega_m}{2} \nabla \left[ \phi_\mathrm{PM}(\mathbf{x}) \right]

Particle Mesh to N-body

F_\theta(\mathbf{x},a) = \frac{3 \Omega_m}{2} \nabla \left[ \phi_\mathrm{PM}(\mathbf{x}) + \phi_\theta (\mathbf{x},\delta,\phi_\mathrm{PM},a) \right]

arXiv:2207.05509

Low Res Potential

True Potential

\delta

Corrected Potential

True Potential

\delta

We can't model galaxy formation, how do we make our models robust?

(\theta_\mathrm{sims}, x_\mathrm{sims}: \small{\mathrm{linear}})
x_\mathrm{obs}: \small{\mathrm{nonlinear}}

Increase the evidence of the observations

Robust Summarisation

\theta_\mathrm{obs} \mathrm{?}
\mathcal{L} = p(\theta_\mathrm{sims}|S(x_\mathrm{sims})) + \lambda p_\mathrm{sims}(S(x_\mathrm{obs}))
\mathcal{L} = p(\theta_\mathrm{sims}|S(x_\mathrm{sims}))

What ML can do for cosmology

  • ML to accelerate non-linear predictions and density estimation

 

  • Can ML extract **all** the information that there is at the field-level in the non-linear regime?

 

  • Compare data and simulations, point us to the missing pieces?

cuestalz@mit.edu

Graph Neural Networks in a nutshell

\mathcal{G} = h^{L}_i, e^{L}_{ij} \rightarrow h^{L+1}_i, e^{L+1}_{ij}
e^{L+1}_{ij} = \phi_e(e^L_{ij}, h^L_i, h^L_j)
h^{L+1}_{i} = \phi_h( h^L_i, \mathcal{A}_j e^{L+1}_{ij})

edge embedding

node embedding

e_{ij}
h_i = \{\mathrm{positions}, \mathrm{velocities}...\}
h_j

Invariance vs Equivariance

r
\theta
\phi

Invariance

Scalar interactions

r

Equivariance

What can we do with vectors? 

Tensor products

v_i
v_j
h_0
h_1
h_5
h_4
h_2
h_3
h_6
e_{01}
e_{12}

Node features

Edge features

\mathcal{G} = h^{L}_i, e^{L}_{ij} \rightarrow h^{L+1}_i, e^{L+1}_{ij}
e^{L+1}_{ij} = \phi_e(e^L_{ij}, h^L_i, h^L_j)

edge embedding

h^{L+1}_{i} = \phi_h( h^L_i, \mathcal{A}_j e^{L+1}_{ij})

node embedding

Input

noisy halo properties

Output

noise prediction

Copy of Copy of deck

By carol cuesta

Copy of Copy of deck

  • 158