Introductory description

A galaxy is a system of stars, dust, stellar remnants and other bodies bound by gravity. For example, the Milky Way (our galaxy) is estimated to contain around 300bn stars and at least 100bn planets. Galaxies usually form groups, also bound by their gravitational interaction, and these groups themselves tend to be part of even larger superclusters. In this module, we will see that we can put together appealing and, sometimes quite simple, explanations of what we observe in these complex systems.

Module web page

Module aims

Outline syllabus

This is an indicative module outline only to give an indication of the sort of topics that may be covered. Actual sessions held may differ.

1. Galaxy classification; the Hubble Tuning Fork; elliptical and spiral galaxies; surface
   brightness profiles.
2. The Milky Way, its structure and properties; the role of stellar populations and the
   interstellar medium.
3. Galaxy populations; luminosity functions, star formation vs AGN, radio galaxies and
   seyferts.
4. Galaxy kinematics; Tully-Fisher relation; rotation curves; dark matter; virial mass
5. The role and origin of dust and gas in galaxies; dust extinction laws; types of dusty galaxies
6. Introduction to galaxies at large scale: the Local Group and nearby clusters

Learning outcomes

By the end of the module, students should be able to:

• Describe the structure of our own Galaxy and how it fits into the ‘zoo’ of galaxies distributed through the Universe;
• Explain the physical principles behind the observations used to study galaxies
• Discuss the outstanding problems in the study of galaxies including the nature of galaxy cores and the roles of dark matter and dust

Indicative reading list

S Philipps, The Structure and Evolution of Galaxies, Wiley, 2005

View reading list on Talis Aspire

Subject specific skills

Knowledge of mathematics and physics. Skills in modelling, reasoning, thinking.

Transferable skills

Analytical, communication, problem-solving, self-study