# Table of contents

1. Lecture notes and useful resources 2. Problem sets 3. About the numerical project and all the tools provided

- Milestone I: Background Cosmology
- Milestone II: Recombination History
- Milestone III: Evolution of structure in the Universe
- Milestone IV: The CMB and matter power-spectra
- How to write the report and grading

4. Slack group you can join to ask questions/get help

# About the course

In this course you will learn about the large scale structure and the Cosmic Microwave Background (CMB) fluctuations: what is the underlying theory and the different physical effects that leads to observable signatures. We follow Dodelson, but provide online lecture notes and problems so its possible to follow it without having the textbook. You will not just learn how to do the theory, but also how to code up the equations to make your own Einstein-Boltzmann solver that computes predictions that can be compared with actual observations. These things are already coded up for you in great packages like CAMB and CLASS which are flexible, full of features and is more accurate and runs faster than you will be able to do in this project (though its possible to get pretty close). But by doing it yourself you get experience in writing a bigger code and with this in hand you can easily explore the consequence of changing the cosmological parameters or turning on/off some of the physics and see how that affects the result to better understand the physics. We will also go through how to structure a code like this, how to test it and make sure it works correctly and the relevant algorithms you need to know to do it efficiently. All these things - knowing the theory, understanding the physics and be able to numerically solve for the predictions - are important to know to be a good cosmologist in the era of precision cosmology.