  What is the connection between how the dark matter was produced in the early
universe and how we can detect it today? Where does the WIMP miracle come from,
and is it really a "WIMP" miracle? What brackets the mass range for thermal
relics? Where does <\sigma v> come from, and what does it mean? What is the
difference between chemical and kinetic decoupling? Why do some people think
that dark matter cannot be lighter than 40 GeV? Why is b\bar b such a popular
annihilation final state? Why is antimatter a good way to look for dark matter?
Why should the cosmic-ray positron fraction decline with energy, and why does
it not? How does one calculate the flux of neutrinos from dark matter
annihilation in a celestial body, and when is that flux independent of the dark
matter pair-annihilation rate? How does dark matter produce photons? Read these
lecture notes, do the suggested 10 exercises, and you will find answers to all
of these questions (and to many more on what You Always Wanted to Know About
Dark Matter But Were Afraid to Ask).
