  This is a course on cosmic microwave background (CMB) anisotropies in the
standard cosmological model, designed for beginning graduate students and
advanced undergraduates. ``Standard cosmological model'' in this context means
a Universe dominated by some form of cold dark matter (CDM) with adiabatic
perturbations generated at some initial epoch, e.g., Inflation, and left to
evolve under gravity alone (which distinguishes it from defect models). The
course is primarily theoretical and concerned with the physics of CMB
anisotropies in this context and their relation to structure formation. Brief
presentations of the uniform Big Bang model and of the observed large--scale
structure of the Universe are given. The bulk of the course then focuses on the
evolution of small perturbations to the uniform model and on the generation of
temperature anisotropies in the CMB. The theoretical development is performed
in the (pseudo--)Newtonian gauge because it aids intuitive understanding by
providing a quick reference to classical (Newtonian) concepts. The fundamental
goal of the course is not to arrive at a highly exact nor exhaustive
calculation of the anisotropies, but rather to a good understanding of the
basic physics that goes into such calculations.
