Carol Cuesta-Lazaro (IAIFI Fellow)
in collaboration with Siddarth Mishra-Sharma and Tess Smidt
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Diffusion Models for Cosmology
Bridging simulations and observations of the Universe
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Initial Conditions of the Universe
Laws of gravity
3-D distribution of galaxies
Which are the ICs of OUR Universe?
What is the origin of these fluctuations?
Probe Inflation
Galaxy formation
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3-D distribution of dark matter
Is GR modified on large scales?
How do galaxies form?
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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
![](https://newscenter.lbl.gov/wp-content/uploads/2022/01/allframe-1000mpc-960x540-1.gif)
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Reverse diffusion: Denoise previous step
Forward diffusion: Add Gaussian noise (fixed)
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Diffusion models
A person half Yoda half Gandalf
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Diffusion on 6D coordinates
Reverse diffusion: Denoise previous step
Forward diffusion: Add Gaussian noise (fixed)
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Cosmology
Tractable likelihood!
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![](https://github.com/smsharma/set-diffuser/blob/main/notebooks/plots/animation_both_norotate.gif?raw=true)
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Setting tight constraints with only 5000 galaxies
All learnable functions
Equivariant functions
Data constraints
Credit: Adapted from Tess Smidt
Equivariant diffusion
Implications for robustness and interpretability?
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+ Galaxy formation
+ Observational systematics (Cut-sky, Fiber collisions)
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Forward Model
N-body simulations
Observations
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https://arxiv.org/pdf/1611.08606.pdf
Is the model robust to systematic errors?
How are simulations and data different?
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deck
By carol cuesta
deck
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